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173 results on '"Sakai N"'

1. FAUST XIII. Dusty cavity and molecular shock driven by IRS7B in the Corona Australis cluster

Author

Sabatini, G., Podio, L., Codella, C., Watanabe, Y., De Simone, M., Bianchi, E., Ceccarelli, C., Chandler, C. J., Sakai, N., Svoboda, B., Testi, L., Aikawa, Y., Balucani, N., Bouvier, M., Caselli, P., Caux, E., Chahine, L., Charnley, S., Cuello, N., Dulieu, F., Evans, L., Fedele, D., Feng, S., Fontani, F., Hama, T., Hanawa, T., Herbst, E., Hirota, T., Isella, A., Jímenez-Serra, I., Johnstone, D., Lefloch, B., Gal, R. Le, Loinard, L., Liu, H. Baobab, López-Sepulcre, A., Maud, L. T., Maureira, M. J., Menard, F., Miotello, A., Moellenbrock, G., Nomura, H., Oba, Y., Ohashi, S., Okoda, Y., Oya, Y., Pineda, J., Rimola, A., Sakai, T., Segura-Cox, D., Shirley, Y., Vastel, C., Viti, S., Watanabe, N., Zhang, Y., Zhang, Z. E., Yamamoto, S., Sabatini, G., Podio, L., Codella, C., Watanabe, Y., De Simone, M., Bianchi, E., Ceccarelli, C., Chandler, C. J., Sakai, N., Svoboda, B., Testi, L., Aikawa, Y., Balucani, N., Bouvier, M., Caselli, P., Caux, E., Chahine, L., Charnley, S., Cuello, N., Dulieu, F., Evans, L., Fedele, D., Feng, S., Fontani, F., Hama, T., Hanawa, T., Herbst, E., Hirota, T., Isella, A., Jímenez-Serra, I., Johnstone, D., Lefloch, B., Gal, R. Le, Loinard, L., Liu, H. Baobab, López-Sepulcre, A., Maud, L. T., Maureira, M. J., Menard, F., Miotello, A., Moellenbrock, G., Nomura, H., Oba, Y., Ohashi, S., Okoda, Y., Oya, Y., Pineda, J., Rimola, A., Sakai, T., Segura-Cox, D., Shirley, Y., Vastel, C., Viti, S., Watanabe, N., Zhang, Y., Zhang, Z. E., and Yamamoto, S.

Abstract

The origin of the chemical diversity observed around low-mass protostars probably resides in the earliest history of these systems. We aim to investigate the impact of protostellar feedback on the chemistry and grain growth in the circumstellar medium of multiple stellar systems. In the context of the ALMA Large Program FAUST, we present high-resolution (50 au) observations of CH$_3$OH, H$_2$CO, and SiO and continuum emission at 1.3 mm and 3 mm towards the Corona Australis star cluster. Methanol emission reveals an arc-like structure at $\sim$1800 au from the protostellar system IRS7B along the direction perpendicular to the major axis of the disc. The arc is located at the edge of two elongated continuum structures that define a cone emerging from IRS7B. The region inside the cone is probed by H$_2$CO, while the eastern wall of the arc shows bright emission in SiO, a typical shock tracer. Taking into account the association with a previously detected radio jet imaged with JVLA at 6 cm, the molecular arc reveals for the first time a bow shock driven by IRS7B and a two-sided dust cavity opened by the mass-loss process. For each cavity wall, we derive an average H$_2$ column density of $\sim$7$\times$10$^{21}$ cm$^{-2}$, a mass of $\sim$9$\times$10$^{-3}$ M$_\odot$, and a lower limit on the dust spectral index of $1.4$. These observations provide the first evidence of a shock and a conical dust cavity opened by the jet driven by IRS7B, with important implications for the chemical enrichment and grain growth in the envelope of Solar System analogues., Comment: 12 pages, 8 figures, 3 tables. Accepted Letter in Astronomy & Astrophysics

Published
2024

2. FAUST XI: Enhancement of the complex organic material in the shocked matter surrounding the [BHB2007] 11 protobinary system

Author

Vastel, C., Sakai, T., Ceccarelli, C., Jiménez-Serra, I., Alves, F., Balucani, N., Bianchi, E., Bouvier, M., Caselli, P., Chandler, C. J., Charnley, S., Codella, C., De Simone, M., Dulieu, F., Evans, L., Fontani, F., Lefloch, B., Loinard, L., Menard, F., Podio, L., Sabatini, G., Sakai, N., Yamamoto, S., Vastel, C., Sakai, T., Ceccarelli, C., Jiménez-Serra, I., Alves, F., Balucani, N., Bianchi, E., Bouvier, M., Caselli, P., Chandler, C. J., Charnley, S., Codella, C., De Simone, M., Dulieu, F., Evans, L., Fontani, F., Lefloch, B., Loinard, L., Menard, F., Podio, L., Sabatini, G., Sakai, N., and Yamamoto, S.

Abstract

iCOMs are species commonly found in the interstellar medium. They are believed to be crucial seed species for the build-up of chemical complexity in star forming regions as well as our own Solar System. Thus, understanding how their abundances evolve during the star formation process and whether it enriches the emerging planetary system is of paramount importance. We use data from the ALMA Large Program FAUST to study the compact line emission towards the [BHB2007] 11 proto-binary system (sources A and B), where a complex structure of filaments connecting the two sources with a larger circumbinary disk has previously been detected. More than 45 CH3OCHO lines are clearly detected, as well as 8 CH3OCH3 transitions , 1 H2CCO transition and 4 t-HCOOH transitions. We compute the abundance ratios with respect to CH3OH for CH3OCHO, CH3OCH3, H2CCO, t-HCOOH (as well as an upper limit for CH3CHO) through a radiative transfer analysis. We also report the upper limits on the column densities of nitrogen bearing iCOMs, N(C2H5CN) and N(C2H3CN). The emission from the detected iCOMs and their precursors is compact and encompasses both protostars, which are separated by only 0.2" (~ 28 au). The integrated intensities tend to align with the Southern filament, revealed by the high spatial resolution observations of the dust emission at 1.3 mm. A PV and 2D analysis are performed on the strongest and uncontaminated CH3OCH3 transition and show three different spatial and velocity regions, two of them being close to 11B (Southern filament) and the third one near 11A. All our observations suggest that the detected methanol, as well as the other iCOMs, are generated by the shocked gas from the incoming filaments streaming towards [BHB2007] 11A and 11B, respectively, making this source one of the few where chemical enrichment of the gas caused by the streaming material is observed., Comment: Accepted in A&A

Published
2024

3. FAUST XII. Accretion streamers and jets in the VLA 1623--2417 protocluster

Author

Codella, C., Podio, L., De Simone, M., Ceccarelli, C., Ohashi, S., Chandler, C. J., Sakai, N., Pineda, J. E., Segura-Cox, D. M., Bianchi, E., Cuello, N., López-Sepulcre, A., Fedele, D., Caselli, P., Charnley, S., Johnstone, D., Zhang, Z. E., Maureira, M. J., Zhang, Y., Sabatini, G., Svoboda, B., Jiménez-Serra, I., Loinard, L., Mercimek, S., Murillo, N., Yamamoto, S., Codella, C., Podio, L., De Simone, M., Ceccarelli, C., Ohashi, S., Chandler, C. J., Sakai, N., Pineda, J. E., Segura-Cox, D. M., Bianchi, E., Cuello, N., López-Sepulcre, A., Fedele, D., Caselli, P., Charnley, S., Johnstone, D., Zhang, Z. E., Maureira, M. J., Zhang, Y., Sabatini, G., Svoboda, B., Jiménez-Serra, I., Loinard, L., Mercimek, S., Murillo, N., and Yamamoto, S.

Abstract

The ALMA interferometer has played a key role in revealing a new component of the Sun-like star forming process: the molecular streamers, i.e. structures up to thousands of au long funneling material non-axisymmetrically to disks. In the context of the FAUST ALMA LP, the archetypical VLA1623-2417 protostellar cluster has been imaged at 1.3 mm in the SO(5$_6$--4$_5$), SO(6$_6$--5$_5$), and SiO(5--4) line emission at the spatial resolution of 50 au. We detect extended SO emission, peaking towards the A and B protostars. Emission blue-shifted down to 6.6 km s$^{-1}$ reveals for the first time a long ($\sim$ 2000 au) accelerating streamer plausibly feeding the VLA1623 B protostar. Using SO, we derive for the first time an estimate of the excitation temperature of an accreting streamer: 33$\pm$9 K. The SO column density is $\sim$ 10$^{14}$ cm$^{-2}$, and the SO/H$_2$ abundance ratio is $\sim$ 10$^{-8}$. The total mass of the streamer is 3 $\times$ 10$^{-3}$ $Msun$, while its accretion rate is 3--5 $\times$ 10$^{-7}$ Msun yr$^{-1}$. This is close to the mass accretion rate of VLA1623 B, in the 0.6--3 $\times$ 10$^{-7}$ Msun yr$^{-1}$ range, showing the importance of the streamer in contributing to the mass of protostellar disks. The highest blue- and red-shifted SO velocities behave as the SiO(5--4) emission, the latter species detected for the first time in VLA1623-2417: the emission is compact (100-200 au), and associated only with the B protostar. The SO excitation temperature is $\sim$ 100 K, supporting the occurrence of shocks associated with the jet, traced by SiO., Comment: accepted by MNRAS

Published
2024

4. Long-term multisystemic efficacy of migalastat on Fabry-associated clinical events, including renal, cardiac and cerebrovascular outcomes

Author

Hughes, DA, Bichet, DG, Giugliani, R, Hopkin, RJ, Krusinska, E, Nicholls, K, Olivotto, I, Feldt-Rasmussen, U, Sakai, N, Skuban, N, Sunder-Plassmann, G, Torra, R, Wilcox, WR, Hughes, DA, Bichet, DG, Giugliani, R, Hopkin, RJ, Krusinska, E, Nicholls, K, Olivotto, I, Feldt-Rasmussen, U, Sakai, N, Skuban, N, Sunder-Plassmann, G, Torra, R, and Wilcox, WR

Abstract

BACKGROUND: Fabry disease is a rare, multisystemic disorder caused by GLA gene variants that lead to alpha galactosidase A deficiency, resulting in accumulation of glycosphingolipids and cellular dysfunction. Fabry-associated clinical events (FACEs) cause significant morbidity and mortality, yet the long-term effect of Fabry therapies on FACE incidence remains unclear. METHODS: This posthoc analysis evaluated incidence of FACEs (as a composite outcome and separately for renal, cardiac and cerebrovascular events) in 97 enzyme replacement therapy (ERT)-naïve and ERT-experienced adults with Fabry disease and amenable GLA variants who were treated with migalastat for up to 8.6 years (median: 5 years) in Phase III clinical trials of migalastat. Associations between baseline characteristics and incidence of FACEs were also evaluated. RESULTS: During long-term migalastat treatment, 17 patients (17.5%) experienced 22 FACEs and there were no deaths. The incidence rate of FACEs was 48.3 events per 1000 patient-years overall. Numerically higher incidence rates were observed in men versus women, patients aged >40 years versus younger patients, ERT-naïve versus ERT-experienced patients and men with the classic phenotype versus men and women with all other phenotypes. There was no statistically significant difference in time to first FACE when analysed by patient sex, phenotype, prior treatment status or age. Lower baseline estimated glomerular filtration rate (eGFR) was associated with an increased risk of FACEs across patient populations. CONCLUSIONS: The overall incidence of FACEs for patients during long-term treatment with migalastat compared favourably with historic reports involving ERT. Lower baseline eGFR was a significant predictor of FACEs.

Published
2023

5. FAUST – VIII. The protostellar disc of VLA 1623–2417W and its streamers imaged by ALMA

Author

European Commission, European Research Council, Ministry of Education, Culture, Sports, Science and Technology (Japan), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Consejo Nacional de Ciencia y Tecnología (México), German Research Foundation, National Research Council of Canada, Natural Sciences and Engineering Research Council of Canada, Mercimek, Seyma, Podio, L., Codella, Claudio, Chahine, L., López-Sepulcre, A., Ohashi, S., Loinard, L., Johnstone, Doug, Menard, F., Cuello, N., Caselli, Paola, Zamponi, Joaquin, Aikawa, Y., Bianchi, E., Busquet, Gemma, Pineda, Jaime E., Bouvier, Mathilde, De Simone, Marta, Zhang, Y., Sakai, N., Chandler, C. J., Ceccarelli, Cecilia, Alves, F., Durán, A., Fedele, D., Murillo, Nadia, Jiménez-Serra, Izaskun, Yamamoto, Satoshi, European Commission, European Research Council, Ministry of Education, Culture, Sports, Science and Technology (Japan), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Consejo Nacional de Ciencia y Tecnología (México), German Research Foundation, National Research Council of Canada, Natural Sciences and Engineering Research Council of Canada, Mercimek, Seyma, Podio, L., Codella, Claudio, Chahine, L., López-Sepulcre, A., Ohashi, S., Loinard, L., Johnstone, Doug, Menard, F., Cuello, N., Caselli, Paola, Zamponi, Joaquin, Aikawa, Y., Bianchi, E., Busquet, Gemma, Pineda, Jaime E., Bouvier, Mathilde, De Simone, Marta, Zhang, Y., Sakai, N., Chandler, C. J., Ceccarelli, Cecilia, Alves, F., Durán, A., Fedele, D., Murillo, Nadia, Jiménez-Serra, Izaskun, and Yamamoto, Satoshi

Abstract

More than 50 per cent of solar-mass stars form in multiple systems. It is therefore crucial to investigate how multiplicity affects the star and planet formation processes at the protostellar stage. We report continuum and C18O (2–1) observations of the VLA 1623–2417 protostellar system at 50 au angular resolution as part of the ALMA (Atacama Large Millimeter/submillimeter Array) Large Program FAUST. The 1.3 mm continuum probes the discs of VLA 1623A, B, and W, and the circumbinary disc of the A1 + A2 binary. The C18O emission reveals, for the first time, the gas in the disc envelope of VLA 1623W. We estimate the dynamical mass of VLA 1623W, Mdyn = 0.45 ± 0.08 M⊙, and the mass of its disc, Mdisc ∼ 6 × 10−3 M⊙. C18O also reveals streamers that extend up to 1000 au, spatially and kinematically connecting the envelope and outflow cavities of the A1 + A2 + B system with the disc of VLA 1623W. The presence of the streamers, as well as the spatial (∼1300 au) and velocity (∼2.2 km s−1) offsets of VLA 1623W, suggests that either sources W and A + B formed in different cores, interacting between them, or source W has been ejected from the VLA 1623 multiple system during its formation. In the latter case, the streamers may funnel material from the envelope and cavities of VLA 1623AB on to VLA 1623W, thus concurring to set its final mass and chemical content.

Published
2023

6. The Perseus ALMA Chemical Survey (PEACHES). III. Sulfur-bearing species tracing accretion and ejection processes in young protostars

Author

de la Villarmois, E. Artur, Guzman, V. V., Yang, Y. -L., Zhang, Y., Sakai, N., de la Villarmois, E. Artur, Guzman, V. V., Yang, Y. -L., Zhang, Y., and Sakai, N.

Abstract

(Abridged) Sulfur chemistry is poorly understood in the process of low-mass star and planet formation, where the main carriers of sulfur are still unknown. Despite the fact that simple S-bearing molecules are usually detected toward embedded sources, large surveys of S-bearing molecules with high angular resolution and sensitive observations are currently lacking. The goal of this work is to present an unbiased survey of simple sulfur-bearing species in protostars and provide new statistics. In addition, we investigate the role of S-bearing molecules in accretion processes and the connection between (non-)detection of complex organic molecules (COMs) and S-related species. We present the observations of sulfur-bearing species that are part of the Perseus ALMA Chemical Survey (PEACHES). We analyzed a total of 50 Class 0/I sources with an average angular resolution of about 0.6" (~180 au) in ALMA band 6. We present detection rates for CS, SO, 34SO, and SO2. The SO/34SO ratio is lower than the canonical value of 22 and the lowest values are found for those sources rich in COMs. This ratio, therefore, seems to be a good tracer of the inner high-density envelope. The detection of multiple COMs seems to be related to the presence of collimated outflows and SO2 emission seems to trace the warm gas in those sources where CH3OH is also detected. The SO2 abundances toward the PEACHES sample are, on average, two orders of magnitude lower than values from the Ophiuchus star-forming region and comparable with sources in Taurus, suggesting that the sulfur depletion in the gas-phase could depend on the external UV radiation. Finally, the SO2 emission detected in different evolutionary stages seems to arise from different physical mechanisms: high column density of warm material in Class 0 sources, shocks in Class I/II, and exposure to UV radiation from the protostar in more evolved Class II disks., Comment: 31 pages, 17 Figures (including appendix)

Published
2023
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7. FAUST IX. Multi-band, multi-scale dust study of L1527 IRS. Evidence for dust properties variations within the envelope of a Class 0/I YSO

Author

Cacciapuoti, L., Macias, E., Maury, A. J., Chandler, C. J., Sakai, N., Tychoniec, Ł., Viti, S., Natta, A., De Simone, M., Miotello, A., Codella, C., Ceccarelli, C., Podio, L., Fedele, D., Johnstone, D., Shirley, Y., Liu, B. J., Bianchi, E., Zhang, Z. E., Pineda, J., Loinard, L., Ménard, F., Lebreuilly, U., Klessen, R. S., Hennebelle, P., Molinari, S., Testi, L., Yamamoto, S., Cacciapuoti, L., Macias, E., Maury, A. J., Chandler, C. J., Sakai, N., Tychoniec, Ł., Viti, S., Natta, A., De Simone, M., Miotello, A., Codella, C., Ceccarelli, C., Podio, L., Fedele, D., Johnstone, D., Shirley, Y., Liu, B. J., Bianchi, E., Zhang, Z. E., Pineda, J., Loinard, L., Ménard, F., Lebreuilly, U., Klessen, R. S., Hennebelle, P., Molinari, S., Testi, L., and Yamamoto, S.

Abstract

Early dust grain growth in protostellar envelopes infalling on young discs has been suggested in recent studies, supporting the hypothesis that dust particles start to agglomerate already during the Class 0/I phase of young stellar objects (YSOs). If this early evolution were confirmed, it would impact the usually assumed initial conditions of planet formation, where only particles with sizes $\lesssim 0.25 \mu$m are usually considered for protostellar envelopes. We aim to determine the maximum grain size of the dust population in the envelope of the Class 0/I protostar L1527 IRS, located in the Taurus star-forming region (140 pc). We use Atacama Large millimetre/sub-millimetre Array (ALMA) and Atacama Compact Array (ACA) archival data and present new observations, in an effort to both enhance the signal-to-noise ratio of the faint extended continuum emission and properly account for the compact emission from the inner disc. Using observations performed in four wavelength bands and extending the spatial range of previous studies, we aim to place tight constraints on the spectral ($\alpha$) and dust emissivity ($\beta$) indices in the envelope of L1527 IRS. We find a rather flat $\alpha \sim$ 3.0 profile in the range 50-2000 au. Accounting for the envelope temperature profile, we derive values for the dust emissivity index, 0.9 < $\beta$ < 1.6, and reveal a tentative, positive outward gradient. This could be interpreted as a distribution of mainly ISM-like grains at 2000 au, gradually progressing to (sub-)millimetre-sized dust grains in the inner envelope, where at R=300 au, $\beta$ = 1.1 +/- 0.1. Our study supports a variation of the dust properties in the envelope of L1527 IRS. We discuss how this can be the result of in-situ grain growth, dust differential collapse from the parent core, or upward transport of disc large grains., Comment: Accepted for publication in A&A. Contains 18 pages, 21 figures, 5 tables Replacement on Nov 22 to change title number of FAUST series from "X" to "IX."

Published
2023
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8. A Keplerian disk with a four-arm spiral birthing an episodically accreting high-mass protostar

Author

Burns, R. A., Uno, Y., Sakai, N., Blanchard, J., Rosli, Z., Orosz, G., Yonekura, Y., Tanabe, Y., Sugiyama, K., Hirota, T., Kim, Kee-Tae, Aberfelds, A., Volvach, A. E., Bartkiewicz, A., Garatti, A. Caratti o, Sobolev, A. M., Stecklum, B., Brogan, C., Phillips, C., Ladeyschikov, D. A., Johnstone, D., Surcis, G., MacLeod, G. C., Linz, H., Chibueze, J. O., Brand, J., Eislöffel, J., Hyland, L., Uscanga, L., Olech, M., Durjasz, M., Bayandina, O., Breen, S., Ellingsen, S. P., Heever, S. P. van den, Hunter, T. R., Chen, X., Burns, R. A., Uno, Y., Sakai, N., Blanchard, J., Rosli, Z., Orosz, G., Yonekura, Y., Tanabe, Y., Sugiyama, K., Hirota, T., Kim, Kee-Tae, Aberfelds, A., Volvach, A. E., Bartkiewicz, A., Garatti, A. Caratti o, Sobolev, A. M., Stecklum, B., Brogan, C., Phillips, C., Ladeyschikov, D. A., Johnstone, D., Surcis, G., MacLeod, G. C., Linz, H., Chibueze, J. O., Brand, J., Eislöffel, J., Hyland, L., Uscanga, L., Olech, M., Durjasz, M., Bayandina, O., Breen, S., Ellingsen, S. P., Heever, S. P. van den, Hunter, T. R., and Chen, X.

Abstract

High-mass protostars (M$_{\star} >$ 8 M$_{\odot}$) are thought to gain the majority of their mass via short, intense bursts of growth. This episodic accretion is thought to be facilitated by gravitationally unstable and subsequently inhomogeneous accretion disks. Limitations of observational capabilities, paired with a lack of observed accretion burst events has withheld affirmative confirmation of the association between disk accretion, instability and the accretion burst phenomenon in high-mass protostars. Following its 2019 accretion burst, a heat-wave driven by a burst of radiation propagated outward from the high-mass protostar G358.93-0.03-MM1. Six VLBI (very long baseline interferometry) observations of the raditively pumped 6.7 GHz methanol maser were conducted during this period, tracing ever increasing disk radii as the heat-wave propagated outward. Concatenating the VLBI maps provided a sparsely sampled, milliarcsecond view of the spatio-kinematics of the accretion disk covering a physical range of $\sim$ 50 - 900 AU. We term this observational approach `heat-wave mapping'. We report the discovery of a Keplerian accretion disk with a spatially resolved four-arm spiral pattern around G358.93-0.03-MM1. This result positively implicates disk accretion and spiral arm instabilities into the episodic accretion high-mass star formation paradigm., Comment: Published in Nature Astronomy in 2023

Published
2023
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9. FAUST VIII. The protostellar disk of VLA 1623-2417 W and its streamers imaged by ALMA

Author

Mercimek, S., Podio, L., Codella, C., Chahine, L., López-Sepulcre, A., Ohashi, S., Loinard, L., Johnstone, D., Menard, F., Cuello, N., Caselli, P., Zamponi, J., Aikawa, Y., Bianchi, E., Busquet, G., Pineda, J. E., Bouvier, M., De Simone, M., Zhang, Y., Sakai, N., Chandler, C. J., Ceccarelli, C., Alves, F., Durán, A., Fedele, D., Murillo, N., Jiménez-Serra, I., Yamamoto, S., Mercimek, S., Podio, L., Codella, C., Chahine, L., López-Sepulcre, A., Ohashi, S., Loinard, L., Johnstone, D., Menard, F., Cuello, N., Caselli, P., Zamponi, J., Aikawa, Y., Bianchi, E., Busquet, G., Pineda, J. E., Bouvier, M., De Simone, M., Zhang, Y., Sakai, N., Chandler, C. J., Ceccarelli, C., Alves, F., Durán, A., Fedele, D., Murillo, N., Jiménez-Serra, I., and Yamamoto, S.

Abstract

More than 50% of solar-mass stars form in multiple systems. It is therefore crucial to investigate how multiplicity affects the star and planet formation processes at the protostellar stage. We report continuum and C$^{18}$O (2-1) observations of the VLA 1623-2417 protostellar system at 50 au angular resolution as part of the ALMA Large Program FAUST. The 1.3 mm continuum probes the disks of VLA 1623A, B, and W, and the circumbinary disk of the A1+A2 binary. The C$^{18}$O emission reveals, for the first time, the gas in the disk-envelope of VLA 1623W. We estimate the dynamical mass of VLA 1623W, $M_{\rm dyn}=0.45\pm0.08$ M$_{\odot}$, and the mass of its disk, $M_{\rm disk}\sim6\times10^{-3}$ M$_{\odot}$. C$^{18}$O also reveals streamers that extend up to 1000 au, spatially and kinematically connecting the envelope and outflow cavities of the A1+A2+B system with the disk of VLA 1623W. The presence of the streamers, as well as the spatial ($\sim$1300 au) and velocity ($\sim$2.2 km/s) offset of VLA 1623W suggest that either sources W and A+B formed in different cores, interacting between them, or that source W has been ejected from the VLA 1623 multiple system during its formation. In the latter case, the streamers may funnel material from the envelope and cavities of VLA 1623AB onto VLA 1623W, thus concurring to set its final mass and chemical content., Comment: 10 pages, 5 figures, accepted by MNRAS

Published
2023
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10. Global impact of the COVID-19 pandemic on subarachnoid haemorrhage hospitalisations, aneurysm treatment and in-hospital mortality: 1-year follow-up

Author

Nguyen, T.N. Qureshi, M.M. Klein, P. Yamagami, H. Mikulik, R. Etminan, N. Abdalkader, M. Mansour, O.Y. Czlonkowska, A. Lo, H. Sathya, A. Demeestere, J. Tsivgoulis, G. Sakai, N. Sedova, P. Kristoffersen, E.S. Mohammaden, M. Lereis, V.P. Scollo, S.D. Ma, A. Rahman, A. Bonnet, T. Cortier, J. Raedt, S.D. Lemmens, R. Ligot, N. Hidalgo, R.C.T. Cuervo, D.L.M. De Oliveira Neves, L. Rezende, M.T.S. Santiago, I.B. Sirakov, A. Sirakov, S. Cora, E.A. Kelly, M.E. Lavoie, P. Peeling, L. Pikula, A. Rivera, R. Chen, H.-S. Chen, Y. Fang, H. Bedekovic, M.R. Budincevic, H. Strossmayer, J.J. Čabal, M. Hrabanovska, E. Jurak, L. Kadlckova, J. Karpowicz, I. Klečka, L. Kovař, M. Neumann, J. Palouškova, H. Reiser, M. Rekova, P. Škorňa, M. Šramek, M. Vitkova, E. Žakova, L. Sobh, K. Alpay, K. Rautio, R. Strbian, D. Gentric, J.-C. Magro, E. Naggara, O. Reiner, P. Abdulazim, A. Bohmann, F.O. Boskamp, S. Gerber, J.C. Kaiser, D.P.O. Kestner, R.I. Mbroh, J. Neyazi, M. Rosenkranz, M. Poli, S. Thomalla, G. Karapanayiotides, T. Kargiotis, O. Koutroulou, I. Palaiodimou, L. Guerra, J.D.B. Huded, V. Nagendra, S. Prajapati, C. Krishna, A. Sani, A.F. Ghoreishi, A. Ilkhchi, R.B. Jalili, J. Sabetay, S.I. Raya, T.A. Acampa, M. Longoni, M. Bigliani, C.R. Castellan, L. Ornello, R. Renieri, L. Romoli, M. Sacco, S. Sangalli, D. Vigano, M. Zini, A. Tokimura, H. Sonoda, K. Todo, K. Fukuda, H. Fujita, K. Sakaguchi, M. Uno, M. Kan, I. Kosuke, M. Kono, R. Kimura, N. Yamamoto, N. Yamamoto, R. Doijiri, R. Shindo, S. Ohara, N. Imamura, H. Ogawa, T. Uwatoko, T. Kanamaru, T. Fujinaka, T. Takenobu, Y. Toyoda, K. Matsumaru, Y. Yazawa, Y. Sugiura, Y. Baek, J.-H. Kwon, Y.S. Lee, Y.H. Seo, K.-D. Sohn, S.-I. Chan, Y.C. Wan Zaidi, W.A. Barrientos-Prieto, J. Gongora-Rivera, F. Martinez-Marino, M. Calderon-Vallejo, A. Groppa, S. Pavel, L. Coutinho, J.M. Dippel, D. Rinkel, L. Van Dam-Nolen, D.H.K. Nwazor, E.O. Sunmonu, T.A. Al Hashmi, A.M. Ahmad, S. Rashid, U. Rodriguez-Kadota, L. Vences, M.A. Yalung, P.M. Dy, J.S.H. Brola, W. Dȩbi and Nguyen, T.N. Qureshi, M.M. Klein, P. Yamagami, H. Mikulik, R. Etminan, N. Abdalkader, M. Mansour, O.Y. Czlonkowska, A. Lo, H. Sathya, A. Demeestere, J. Tsivgoulis, G. Sakai, N. Sedova, P. Kristoffersen, E.S. Mohammaden, M. Lereis, V.P. Scollo, S.D. Ma, A. Rahman, A. Bonnet, T. Cortier, J. Raedt, S.D. Lemmens, R. Ligot, N. Hidalgo, R.C.T. Cuervo, D.L.M. De Oliveira Neves, L. Rezende, M.T.S. Santiago, I.B. Sirakov, A. Sirakov, S. Cora, E.A. Kelly, M.E. Lavoie, P. Peeling, L. Pikula, A. Rivera, R. Chen, H.-S. Chen, Y. Fang, H. Bedekovic, M.R. Budincevic, H. Strossmayer, J.J. Čabal, M. Hrabanovska, E. Jurak, L. Kadlckova, J. Karpowicz, I. Klečka, L. Kovař, M. Neumann, J. Palouškova, H. Reiser, M. Rekova, P. Škorňa, M. Šramek, M. Vitkova, E. Žakova, L. Sobh, K. Alpay, K. Rautio, R. Strbian, D. Gentric, J.-C. Magro, E. Naggara, O. Reiner, P. Abdulazim, A. Bohmann, F.O. Boskamp, S. Gerber, J.C. Kaiser, D.P.O. Kestner, R.I. Mbroh, J. Neyazi, M. Rosenkranz, M. Poli, S. Thomalla, G. Karapanayiotides, T. Kargiotis, O. Koutroulou, I. Palaiodimou, L. Guerra, J.D.B. Huded, V. Nagendra, S. Prajapati, C. Krishna, A. Sani, A.F. Ghoreishi, A. Ilkhchi, R.B. Jalili, J. Sabetay, S.I. Raya, T.A. Acampa, M. Longoni, M. Bigliani, C.R. Castellan, L. Ornello, R. Renieri, L. Romoli, M. Sacco, S. Sangalli, D. Vigano, M. Zini, A. Tokimura, H. Sonoda, K. Todo, K. Fukuda, H. Fujita, K. Sakaguchi, M. Uno, M. Kan, I. Kosuke, M. Kono, R. Kimura, N. Yamamoto, N. Yamamoto, R. Doijiri, R. Shindo, S. Ohara, N. Imamura, H. Ogawa, T. Uwatoko, T. Kanamaru, T. Fujinaka, T. Takenobu, Y. Toyoda, K. Matsumaru, Y. Yazawa, Y. Sugiura, Y. Baek, J.-H. Kwon, Y.S. Lee, Y.H. Seo, K.-D. Sohn, S.-I. Chan, Y.C. Wan Zaidi, W.A. Barrientos-Prieto, J. Gongora-Rivera, F. Martinez-Marino, M. Calderon-Vallejo, A. Groppa, S. Pavel, L. Coutinho, J.M. Dippel, D. Rinkel, L. Van Dam-Nolen, D.H.K. Nwazor, E.O. Sunmonu, T.A. Al Hashmi, A.M. Ahmad, S. Rashid, U. Rodriguez-Kadota, L. Vences, M.A. Yalung, P.M. Dy, J.S.H. Brola, W. Dȩbi

Abstract

Background Prior studies indicated a decrease in the incidences of aneurysmal subarachnoid haemorrhage (aSAH) during the early stages of the COVID-19 pandemic. We evaluated differences in the incidence, severity of aSAH presentation, and ruptured aneurysm treatment modality during the first year of the COVID-19 pandemic compared with the preceding year. Methods We conducted a cross-sectional study including 49 countries and 187 centres. We recorded volumes for COVID-19 hospitalisations, aSAH hospitalisations, Hunt-Hess grade, coiling, clipping and aSAH in-hospital mortality. Diagnoses were identified by International Classification of Diseases, 10th Revision, codes or stroke databases from January 2019 to May 2021. Results Over the study period, there were 16 247 aSAH admissions, 344 491 COVID-19 admissions, 8300 ruptured aneurysm coiling and 4240 ruptured aneurysm clipping procedures. Declines were observed in aSAH admissions (-6.4% (95% CI-7.0% to-5.8%), p=0.0001) during the first year of the pandemic compared with the prior year, most pronounced in high-volume SAH and high-volume COVID-19 hospitals. There was a trend towards a decline in mild and moderate presentations of subarachnoid haemorrhage (SAH) (mild:-5% (95% CI-5.9% to-4.3%), p=0.06; moderate:-8.3% (95% CI-10.2% to-6.7%), p=0.06) but no difference in higher SAH severity. The ruptured aneurysm clipping rate remained unchanged (30.7% vs 31.2%, p=0.58), whereas ruptured aneurysm coiling increased (53.97% vs 56.5%, p=0.009). There was no difference in aSAH in-hospital mortality rate (19.1% vs 20.1%, p=0.12). Conclusion During the first year of the pandemic, there was a decrease in aSAH admissions volume, driven by a decrease in mild to moderate presentation of aSAH. There was an increase in the ruptured aneurysm coiling rate but neither change in the ruptured aneurysm clipping rate nor change in aSAH in-hospital mortality. Trial registration number NCT04934020. © Author(s) (or their employer(s)) 2022. No com

Published
2022

11. Mass ejection and time variability in protostellar outflows: Cep E. SOLIS XVI

Author

Schutzer, A. de A., Rivera-Ortiz, P. R., Lefloch, B., Gusdorf, A., Favre, C., Segura-Cox, D., Lopez-Sepulcre, A., Neri, R., Ospina-Zamudio, J., De Simone, M., Codella, C., Viti, S., Podio, L., Pineda, J., O'Donoghue, R., Ceccarelli, C., Caselli, P., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Bottinelli, S., Caux, E., Chacón-Tanarro, A., Dulieu, F., Enrique-Romero, J., Fontani, F., Feng, S., Holdship, J., Jiménez-Serra, I., Al-Edhari, A. Jaber, Kahane, C., Lattanzi, V., Oya, Y., Punanova, A., Rimola, A., Sakai, N., Spezzano, S., Sims, I. R., Taquet, V., Testi, L., Theulé, P., Ugliengo, P., Vastel, C., Vasyunin, A. I., Vazart, F., Yamamoto, S., Witzel, A., Schutzer, A. de A., Rivera-Ortiz, P. R., Lefloch, B., Gusdorf, A., Favre, C., Segura-Cox, D., Lopez-Sepulcre, A., Neri, R., Ospina-Zamudio, J., De Simone, M., Codella, C., Viti, S., Podio, L., Pineda, J., O'Donoghue, R., Ceccarelli, C., Caselli, P., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Bottinelli, S., Caux, E., Chacón-Tanarro, A., Dulieu, F., Enrique-Romero, J., Fontani, F., Feng, S., Holdship, J., Jiménez-Serra, I., Al-Edhari, A. Jaber, Kahane, C., Lattanzi, V., Oya, Y., Punanova, A., Rimola, A., Sakai, N., Spezzano, S., Sims, I. R., Taquet, V., Testi, L., Theulé, P., Ugliengo, P., Vastel, C., Vasyunin, A. I., Vazart, F., Yamamoto, S., and Witzel, A.

Abstract

Protostellar jets are an important agent of star formation feedback, tightly connected with the mass-accretion process. The history of jet formation and mass-ejection provides constraints on the mass accretion history and the nature of the driving source. We want to characterize the time-variability of the mass-ejection phenomena at work in the Class 0 protostellar phase, in order to better understand the dynamics of the outflowing gas and bring more constraints on the origin of the jet chemical composition and the mass-accretion history. We have observed the emission of the CO 2-1 and SO N_J=5_4-4_3 rotational transitions with NOEMA, towards the intermediate-mass Class 0 protostellar system Cep E. The CO high-velocity jet emission reveals a central component associated with high-velocity molecular knots, also detected in SO, surrounded by a collimated layer of entrained gas. The gas layer appears to accelerate along the main axis over a length scale delta_0 ~700 au, while its diameter gradually increases up to several 1000au at 2000au from the protostar. The jet is fragmented into 18 knots of mass ~10^-3 Msun, unevenly distributed between the northern and southern lobes, with velocity variations up to 15 km/s close to the protostar, well below the jet terminal velocities. The knot interval distribution is approximately bimodal with a scale of ~50-80yr close to the protostar and ~150-200yr at larger distances >12". The mass-loss rates derived from knot masses are overall steady, with values of 2.7x10^-5 Msun/yr (8.9x10^-6 Msun/yr) in the northern (southern) lobe. The interaction of the ambient protostellar material with high-velocity knots drives the formation of a molecular layer around the jet, which accounts for the higher mass-loss rate in the north. The jet dynamics are well accounted for by a simple precession model with a period of 2000yr and a mass-ejection period of 55yr., Comment: 13 pages, 9 figures, 3 table. Accepted in A&A

Published
2022

12. The chemical nature of Orion protostars: Are ORANGES different from PEACHES? ORANGES II

Author

Bouvier, M., Ceccarelli, C., López-Sepulcre, A., Sakai, N., Yamamoto, S., Yang, Y. -L., Bouvier, M., Ceccarelli, C., López-Sepulcre, A., Sakai, N., Yamamoto, S., and Yang, Y. -L.

Abstract

Understanding the chemical past of our Sun and how life appeared on Earth is no mean feat. The best strategy we can adopt is to study newborn stars located in an environment similar to the one in which our Sun was born and assess their chemical content. In particular, hot corinos are prime targets since recent studies showed correlations between interstellar Complex Organic Molecules (iCOMs) abundances from hot corinos and comets. The ORion ALMA New GEneration Survey (ORANGES) aims to assess the number of hot corinos in the closest and best analogue to our Sun's birth environment, the OMC-2/3 filament. In this context, we investigated the chemical nature of 19 solar-mass protostars and found that 26\% of our sample sources shows warm methanol emission indicative of hot corinos. Compared to the Perseus low-mass star-forming region, where the PErseus ALMA CHEmistry Survey (PEACHES) detected $\sim 60$\% of hot corinos, the latter seem to be relatively scarce in the OMC-2/3 filament. While this suggests that the chemical nature of protostars in Orion and Perseus is different, improved statistics are needed in order to consolidate this result. If the two regions are truly different, this would indicate that the environment is likely playing a role in shaping the chemical composition of protostars., Comment: 16 pages, 8 figures, Accepted in ApJ

Published
2022
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13. Importance of source structure on complex organics emission. I. Observations of CH$_3$OH from low-mass to high-mass protostars

Author

van Gelder, M. L., Nazari, P., Tabone, B., Ahmadi, A., van Dishoeck, E. F., Beltrán, M. T., Fuller, G. A., Sakai, N., Sánchez-Monge, Á., Schilke, P., Yang, Y. -L., Zhang, Y., van Gelder, M. L., Nazari, P., Tabone, B., Ahmadi, A., van Dishoeck, E. F., Beltrán, M. T., Fuller, G. A., Sakai, N., Sánchez-Monge, Á., Schilke, P., Yang, Y. -L., and Zhang, Y.

Abstract

Complex organic molecules (COMs) are often observed toward embedded Class 0 and I protostars. However, not all Class 0 and I protostars exhibit COMs emission. In this work, variations in methanol (CH$_3$OH) emission are studied to test if absence of CH$_3$OH emission can be linked to source properties. Combining both new and archival observations with ALMA and sources from the literature, a sample of 184 low-mass and high-mass protostars is investigated. The warm (T > 100 K) gaseous CH$_3$OH mass, $M_{\rm CH_3OH}$, is determined for each source using primarily optically thin isotopologues. On average, Class I protostellar systems seem to have less warm $M_{\rm CH_3OH}$ ($<10^{-10}$ M$_\odot$) than younger Class 0 sources ($\sim10^{-7}$ M$_\odot$). High-mass sources in our sample show higher warm $M_{\rm CH_3OH}$ up to $10^{-7}-10^{-3}$ M$_\odot$. To take into account the effect of the source's overall mass on $M_{\rm CH_3OH}$, a normalized CH$_3$OH mass is defined as $M_{\rm CH_3OH}/M_{\rm dust,0}$, where $M_{\rm dust,0}$ is the cold + warm dust mass within a fixed radius. Excluding upper limits, a simple power-law fit to the normalized warm CH$_3$OH masses results in $M_{\rm CH_3OH}/M_{\rm dust,0}\propto L_{\rm bol}^{0.70\pm0.05}$. This is in good agreement with a simple hot core toy model which predicts that the normalized $M_{\rm CH_3OH}$ increases with $L_{\rm bol}^{0.75}$ due to the snowline moving outward. Sources for which the size of the disk is equivalent or smaller than the estimated 100 K radius agree well with the best-fit power-law model, whereas sources with significantly larger disks show up to two orders of magnitude lower normalized warm CH$_3$OH masses. Based on the latter results, we suggest that source structure such as a disk can result in colder gas and thus fewer COMs in the gas phase. Additionally, optically thick dust can hide the emission of COMs., Comment: 22 pages, 6 figures, accepted for publication in A&A

Published
2022

14. Smoking remains associated with education after controlling for social background and genetic factors in a study of 18 twin cohorts

Author

Silventoinen, K, Piirtola, M, Jelenkovic, A, Sund, R, Tarnoki, AD, Tarnoki, DL, Medda, E, Nistico, L, Toccaceli, V, Honda, C, Inui, F, Tomizawa, R, Watanabe, M, Sakai, N, Gatz, M, Butler, DA, Lee, J, Lee, SJ, Sung, J, Franz, CE, Kremen, WS, Lyons, MJ, Derom, CA, Vlietinck, RF, Loos, RJF, Tynelius, P, Rasmussen, F, Martin, NG, Medland, SE, Montgomery, GW, Brandt, I, Nilsen, TS, Harris, JR, Tyler, J, Hopper, JL, Magnusson, PKE, Pedersen, NL, Aslan, AKD, Ordonana, JR, Sanchez-Romera, JF, Colodro-Conde, L, Rebato, E, Zhang, D, Pang, Z, Tan, Q, Silberg, JL, Maes, HH, Boomsma, D, Sorensen, TIA, Korhonen, T, Kaprio, J, Silventoinen, K, Piirtola, M, Jelenkovic, A, Sund, R, Tarnoki, AD, Tarnoki, DL, Medda, E, Nistico, L, Toccaceli, V, Honda, C, Inui, F, Tomizawa, R, Watanabe, M, Sakai, N, Gatz, M, Butler, DA, Lee, J, Lee, SJ, Sung, J, Franz, CE, Kremen, WS, Lyons, MJ, Derom, CA, Vlietinck, RF, Loos, RJF, Tynelius, P, Rasmussen, F, Martin, NG, Medland, SE, Montgomery, GW, Brandt, I, Nilsen, TS, Harris, JR, Tyler, J, Hopper, JL, Magnusson, PKE, Pedersen, NL, Aslan, AKD, Ordonana, JR, Sanchez-Romera, JF, Colodro-Conde, L, Rebato, E, Zhang, D, Pang, Z, Tan, Q, Silberg, JL, Maes, HH, Boomsma, D, Sorensen, TIA, Korhonen, T, and Kaprio, J

Abstract

We tested the causality between education and smoking using the natural experiment of discordant twin pairs allowing to optimally control for background genetic and childhood social factors. Data from 18 cohorts including 10,527 monozygotic (MZ) and same-sex dizygotic (DZ) twin pairs discordant for education and smoking were analyzed by linear fixed effects regression models. Within twin pairs, education levels were lower among the currently smoking than among the never smoking co-twins and this education difference was larger within DZ than MZ pairs. Similarly, education levels were higher among former smoking than among currently smoking co-twins, and this difference was larger within DZ pairs. Our results support the hypothesis of a causal effect of education on both current smoking status and smoking cessation. However, the even greater intra-pair differences within DZ pairs, who share only 50% of their segregating genes, provide evidence that shared genetic factors also contribute to these associations.

Published
2022

15. Importance of source structure on complex organics emission II. Do disks explain lack of methanol emission from low-mass protostars?

Author

van Gelder, M. L., Nazari, P., Tabone, B., Ahmadi, A., van Dishoeck, E. F., Beltran, M. T., Fuller, G. A., Sakai, N., Sanchez-Monge, A., Schilke, P., Yang, Y-L, Zhang, Y., van Gelder, M. L., Nazari, P., Tabone, B., Ahmadi, A., van Dishoeck, E. F., Beltran, M. T., Fuller, G. A., Sakai, N., Sanchez-Monge, A., Schilke, P., Yang, Y-L, and Zhang, Y.

Abstract

Context. The protostellar stage is known to be the richest star formation phase in emission from gaseous complex organic molecules. However, some protostellar systems show little or no millimetre (mm) line emission of such species. This can be interpreted as a low abundance of complex organic molecules. Alternatively, complex species could be present in the system, but are not seen in the gas. Aims. The goal is to investigate the second hypothesis for methanol as the most abundant complex organic molecule in protostellar systems. This work aims to determine how effective dust optical depth is in hiding methanol in the gas, and whether methanol can mainly reside in the ice due to the presence of a disk that lowers the temperatures. Hence, we attempt to answer the question whether the presence of a disk and optically thick dust reduce methanol emission even if methanol and other complex species are abundant in the ices and gas. Methods. Using the radiative transfer code RADMC-3D, we calculated methanol emission lines from an envelope-only model and from an envelope-plus-disk model. We compared the results with each other and with the observations. Methanol gas and ice abundances were parametrised inside and outside of the snow surfaces based on values from observations. Both models included either dust grains with low mm opacity or high mm opacity, and their physical parameters such as envelope mass and disk radius were varied. Results. Methanol emission from the envelope-only model is always stronger than from the envelope-plus-disk model by at least a factor similar to 2 as long as the disk radius is larger than similar to 30 au (for L = 8 L-circle dot). In most cases, this is due to lower temperatures (disk shadowing), which causes the smaller amount of warm (greater than or similar to 70 K) methanol inside the snow surface of the envelope-plus-disk model. The intensities drop by more than an order of magnitude for models including high mm opacity dust grains and d

Published
2022

16. Physical properties of accretion shocks toward the Class I protostellar system Oph-IRS 44

Author

de la Villarmois, E. Artur, Guzman, V. V., Jorgensen, J. K., Kristensen, L. E., Bergin, E. A., Harsono, D., Sakai, N., van Dishoeck, E. F., Yamamoto, S., de la Villarmois, E. Artur, Guzman, V. V., Jorgensen, J. K., Kristensen, L. E., Bergin, E. A., Harsono, D., Sakai, N., van Dishoeck, E. F., and Yamamoto, S.

Abstract

Context. The final outcome and chemical composition of a planetary system depend on its formation history: the physical processes that were involved and the molecular species available at different stages. Physical processes such as accretion shocks are thought to be common in the protostellar phase, where the envelope component is still present, and they can release molecules from the dust to the gas phase, altering the original chemical composition of the disk. Consequently, the study of accretion shocks is essential for a better understanding of the physical processes at disk scales and their chemical output.Aims. The purpose of this work is to assess how the material from the infalling envelope feeds the disk and the chemical consequences thereof, particularly the characteristics of accretion shocks traced by sulfur-related species.Methods. We present high angular resolution observations (0 ''.1, corresponding to 14 au) with the Atacama Large Millimeter/submillimeter Array (ALMA) of the Class I protostar Oph-IRS 44 (also known as YLW 16A). The continuum emission at 0.87 mm is observed, together with sulfur-related species such as SO, SO2, and (SO2)-S-34. The non-local thermodynamic equilibrium (non-LTE) radiative-transfer tool RADEX and the rotational diagram method are employed to assess the physical conditions of the SO2 emitting region.Results. Six lines of SO2, two lines of (SO2)-S-34, and one line of SO are detected toward IRS 44. The emission of all the detected lines peaks at similar to 0 ''.1 (similar to 14 au) from the continuum peak and we find infalling-rotating motions inside 30 au. However, only redshifted emission is seen between 50 and 30 au. Colder and more quiescent material is seen toward an offset region located at a distance of similar to 400 au from the protostar, and we do not find evidence of a Keplerian profile in these data. The SO2 emitting region around the protostar is consistent with dense gas (>= 10(8) cm(

Published
2022

17. Physical properties of accretion shocks toward the Class I protostellar system Oph-IRS 44

Author

de la Villarmois, E. Artur, Guzman, V. V., Jorgensen, J. K., Kristensen, L. E., Bergin, E. A., Harsono, D., Sakai, N., van Dishoeck, E. F., Yamamoto, S., de la Villarmois, E. Artur, Guzman, V. V., Jorgensen, J. K., Kristensen, L. E., Bergin, E. A., Harsono, D., Sakai, N., van Dishoeck, E. F., and Yamamoto, S.

Abstract

Context. The final outcome and chemical composition of a planetary system depend on its formation history: the physical processes that were involved and the molecular species available at different stages. Physical processes such as accretion shocks are thought to be common in the protostellar phase, where the envelope component is still present, and they can release molecules from the dust to the gas phase, altering the original chemical composition of the disk. Consequently, the study of accretion shocks is essential for a better understanding of the physical processes at disk scales and their chemical output.Aims. The purpose of this work is to assess how the material from the infalling envelope feeds the disk and the chemical consequences thereof, particularly the characteristics of accretion shocks traced by sulfur-related species.Methods. We present high angular resolution observations (0 ''.1, corresponding to 14 au) with the Atacama Large Millimeter/submillimeter Array (ALMA) of the Class I protostar Oph-IRS 44 (also known as YLW 16A). The continuum emission at 0.87 mm is observed, together with sulfur-related species such as SO, SO2, and (SO2)-S-34. The non-local thermodynamic equilibrium (non-LTE) radiative-transfer tool RADEX and the rotational diagram method are employed to assess the physical conditions of the SO2 emitting region.Results. Six lines of SO2, two lines of (SO2)-S-34, and one line of SO are detected toward IRS 44. The emission of all the detected lines peaks at similar to 0 ''.1 (similar to 14 au) from the continuum peak and we find infalling-rotating motions inside 30 au. However, only redshifted emission is seen between 50 and 30 au. Colder and more quiescent material is seen toward an offset region located at a distance of similar to 400 au from the protostar, and we do not find evidence of a Keplerian profile in these data. The SO2 emitting region around the protostar is consistent with dense gas (>= 10(8) cm(

Published
2022

18. Physical properties of accretion shocks toward the Class I protostellar system Oph-IRS 44

Author

de la Villarmois, E. Artur, Guzmán, V. V., Jørgensen, J. K., Kristensen, L. E., Bergin, E. A., Harsono, D., Sakai, N., van Dishoeck, E. F., Yamamoto, S., de la Villarmois, E. Artur, Guzmán, V. V., Jørgensen, J. K., Kristensen, L. E., Bergin, E. A., Harsono, D., Sakai, N., van Dishoeck, E. F., and Yamamoto, S.

Abstract

(Abridged) Physical processes such as accretion shocks are thought to be common in the protostellar phase, where the envelope component is still present, and they can release molecules from the dust to the gas phase, altering the original chemical composition of the disk. Consequently, the study of accretion shocks is essential for a better understanding of the physical processes at disk scales and their chemical output. The purpose of this work is to assess the characteristics of accretion shocks traced by sulfur-related species. We present ALMA high angular resolution observations (0.1") of the Class I protostar Oph-IRS 44. The continuum emission at 0.87 mm is observed, together with sulfur-related species such as SO, SO$_{2}$, and $^{34}$SO$_{2}$. Six lines of SO$_{2}$, two lines of $^{34}$SO$_{2}$, and one line of SO are detected toward IRS 44. The emission of all the detected lines peaks at ~0.1" (~14 au) from the continuum peak and we find infalling-rotating motions inside 30 au. However, only redshifted emission is seen between 50 and 30 au. Colder and more quiescent material is seen toward an offset region located at a distance of ~400 au from the protostar, and we do not find evidence of a Keplerian profile in these data. Accretion shocks are the most plausible explanation for the high temperatures, high densities, and velocities found for the SO$_{2}$ emission. When material enters the disk--envelope system, it generates accretion shocks that increase the dust temperature and desorb SO$_{2}$ molecules from dust grains. High-energy SO$_{2}$ transitions (~200 K) seem to be the best tracers of accretion shocks that can be followed up by future higher angular resolution ALMA observations and compared to other species to assess their importance in releasing molecules from the dust to the gas phase., Comment: 16 pages, 16 figures

Published
2022
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19. OMC-2 FIR 4 under the microscope: Shocks, filaments, and a highly collimated jet at 100 au scales

Author

Chahine, L., López-Sepulcre, A., Podio, L., Codella, C., Neri, R., Mercimek, S., De Simone, M., Caselli, P., Ceccarelli, C., Bouvier, M., Sakai, N., Fontani, F., Yamamoto, S., Alves, F. O., Lattanzi, V., Evans, L., Favre, C., Chahine, L., López-Sepulcre, A., Podio, L., Codella, C., Neri, R., Mercimek, S., De Simone, M., Caselli, P., Ceccarelli, C., Bouvier, M., Sakai, N., Fontani, F., Yamamoto, S., Alves, F. O., Lattanzi, V., Evans, L., and Favre, C.

Abstract

Star-forming molecular clouds are characterised by the ubiquity of intertwined filaments. The filaments have been observed in both high- and low-mass star-forming regions, and are thought to split into collections of sonic fibres. The locations where filaments converge are termed hubs, and these are associated with the young stellar clusters. However, the observations of filamentary structures within hubs at distances require a high angular resolution that limits the number of such studies conducted so far. The integral shaped filament of the Orion A molecular cloud is noted for harbouring several hubs within which no filamentary structures have been observed so far. The goal of our study is to investigate the nature of the filamentary structures within one of these hubs, which is the chemically rich hub OMC-2 FIR 4, and to analyse their emission with high density and shock tracers. We observed the OMC-2 FIR 4 proto-cluster using Band 6 of the ALMA in Cycle 4 with an angular resolution of ~0.26"(100 au). We analysed the spatial distribution of dust, the shock tracer SiO, and dense gas tracers (i.e., CH$_{3}$OH, CS, and H$^{13}$CN). We also studied gas kinematics using SiO and CH3OH maps. Our observations for the first time reveal interwoven filamentary structures within OMC-2 FIR 4 that are probed by several tracers. Each filamentary structure is characterised by a distinct velocity as seen from the emission peak of CH$_{3}$OH lines. They also show transonic and supersonic motions. SiO is associated with filaments and also with multiple bow-shock features. In addition, for the first time, we reveal a highly collimated SiO jet (~1$^{\circ}$) with a projected length of ~5200 au from the embedded protostar VLA15. Our study shows that multi-scale observations of these regions are crucial for understanding the accretion processes and flow of material that shapes star formation.

Published
2022
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20. Hot methanol in the [BHB2007] 11 protobinary system: hot corino versus shock origin? : FAUST V

Author

Vastel, C., Alves, F., Ceccarelli, C., Bouvier, M., Jimenez-Serra, I., Sakai, T., Caselli, P., Evans, L., Fontani, F., Gal, R. Le, Chandler, C. J., Svoboda, B., Maud, L., Codella, C., Sakai, N., Lopez-Sepulcre, A., Moellenbrock, G., Aikawa, Y., Balucani, N., Bianchi, E., Busquet, G., Caux, E., Charnley, S., Cuello, N., De Simone, M., Dulieu, F., Duran, A., Fedele, D., Feng, S., Francis, L., Hama, T., Hanawa, T., Herbst, E., Hirota, T., Imai, M., Isella, A., Johnstone, D., Lefloch, B., Loinard, L., Maureira, M., Murillo, N. M., Mercimek, S., Mori, S., Menard, F., Miotello, A., Nakatani, R., Nomura, H., Oba, Y., Ohashi, S., Okoda, Y., Ospina-Zamudio, J., Oya, Y., Pineda, J. E., Podio, L., Rimola, A., Cox, D. Segura, Shirley, Y., Testi, L., Viti, S., Watanabe, N., Watanabe, Y., Witzel, A., Xue, C., Zhang, Y., Zhao, B., Yamamoto, S., Vastel, C., Alves, F., Ceccarelli, C., Bouvier, M., Jimenez-Serra, I., Sakai, T., Caselli, P., Evans, L., Fontani, F., Gal, R. Le, Chandler, C. J., Svoboda, B., Maud, L., Codella, C., Sakai, N., Lopez-Sepulcre, A., Moellenbrock, G., Aikawa, Y., Balucani, N., Bianchi, E., Busquet, G., Caux, E., Charnley, S., Cuello, N., De Simone, M., Dulieu, F., Duran, A., Fedele, D., Feng, S., Francis, L., Hama, T., Hanawa, T., Herbst, E., Hirota, T., Imai, M., Isella, A., Johnstone, D., Lefloch, B., Loinard, L., Maureira, M., Murillo, N. M., Mercimek, S., Mori, S., Menard, F., Miotello, A., Nakatani, R., Nomura, H., Oba, Y., Ohashi, S., Okoda, Y., Ospina-Zamudio, J., Oya, Y., Pineda, J. E., Podio, L., Rimola, A., Cox, D. Segura, Shirley, Y., Testi, L., Viti, S., Watanabe, N., Watanabe, Y., Witzel, A., Xue, C., Zhang, Y., Zhao, B., and Yamamoto, S.

Abstract

Methanol is a ubiquitous species commonly found in the molecular interstellar medium. It is also a crucial seed species for the building-up of the chemical complexity in star forming regions. Thus, understanding how its abundance evolves during the star formation process and whether it enriches the emerging planetary system is of paramount importance. We used new data from the ALMA Large Program FAUST (Fifty AU STudy of the chemistry in the disk/envelope system of Solar-like protostars) to study the methanol line emission towards the [BHB2007] 11 protobinary system (sources A and B), where a complex structure of filaments connecting the two sources with a larger circumbinary disk has been previously detected. Twelve methanol lines have been detected with upper energies in the range [45-537] K along with one 13CH3OH transition. The methanol emission is compact and encompasses both protostars, separated by only 28 au and presents three velocity components, not spatially resolved by our observations, associated with three different spatial regions, with two of them close to 11B and the third one associated with 11A. A non-LTE radiative transfer analysis of the methanol lines concludes that the gas is hot and dense and highly enriched in methanol with an abundance as high as 1e-5. Using previous continuum data, we show that dust opacity can potentially completely absorb the methanol line emission from the two binary objects. Although we cannot firmly exclude other possibilities, we suggest that the detected hot methanol is resulting from the shocked gas from the incoming filaments streaming towards [BHB2007] 11 A and B, respectively. Higher spatial resolution observations are necessary to confirm this hypothesis., Comment: 17 pages, accepted in A&A

Published
2022
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21. FAUST VI. VLA 1623--2417 B: a new laboratory for astrochemistry around protostars on 50 au scale

Author

Codella, C., López-Sepulcre, A., Ohashi, S., Chandler, C. J., De Simone, M., Podio, L., Ceccarelli, C., Sakai, N., Alves, F., Durán, A., Fedele, D., Loinard, L., Mercimek, S., Murillo, N., Bianchi, E., Bouvier, M., Busquet, G., Caselli, P., Dulieu, F., Feng, S., Hanawa, T., Johnstone, D., Lefloch, B., Maud, L. T., Moellenbrock, G., Oya, Y., Svoboda, B., Yamamoto, S., Codella, C., López-Sepulcre, A., Ohashi, S., Chandler, C. J., De Simone, M., Podio, L., Ceccarelli, C., Sakai, N., Alves, F., Durán, A., Fedele, D., Loinard, L., Mercimek, S., Murillo, N., Bianchi, E., Bouvier, M., Busquet, G., Caselli, P., Dulieu, F., Feng, S., Hanawa, T., Johnstone, D., Lefloch, B., Maud, L. T., Moellenbrock, G., Oya, Y., Svoboda, B., and Yamamoto, S.

Abstract

The ALMA interferometer, with its unprecedented combination of high-sensitivity and high-angular resolution, allows for (sub-)mm wavelength mapping of protostellar systems at Solar System scales. Astrochemistry has benefited from imaging interstellar complex organic molecules in these jet-disk systems. Here we report the first detection of methanol (CH3OH) and methyl formate (HCOOCH3) emission towards the triple protostellar system VLA1623-2417 A1+A2+B, obtained in the context of the ALMA Large Program FAUST. Compact methanol emission is detected in lines from Eu = 45 K up to 61 K and 537 K towards components A1 and B, respectively. LVG analysis of the CH3OH lines towards VLA1623-2417 B indicates a size of 0.11-0.34 arcsec (14-45 au), a column density N(CH3OH) = 10^16-10^17 cm-2, kinetic temperature > 170 K, and volume density > 10^8 cm-3. An LTE approach is used for VLA1623-2417 A1, given the limited Eu range, and yields Trot < 135 K. The methanol emission around both VLA1623-2417 A1 and B shows velocity gradients along the main axis of each disk. Although the axial geometry of the two disks is similar, the observed velocity gradients are reversed. The CH3OH spectra from B shows two broad (4-5 km s-1) peaks, which are red- and blue-shifted by about 6-7 km s-1 from the systemic velocity. Assuming a chemically enriched ring within the accretion disk, close to the centrifugal barrier, its radius is calculated to be 33 au. The methanol spectra towards A1 are somewhat narrower (about 4 km s-1), implying a radius of 12-24 au., Comment: MNRAS, in press

Published
2022
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22. Mass ejection and time variability in protostellar outflows: Cep E. SOLIS XVI

Author

Schutzer, A. de A., Rivera-Ortiz, P. R., Lefloch, B., Gusdorf, A., Favre, C., Segura-Cox, D., Lopez-Sepulcre, A., Neri, R., Ospina-Zamudio, J., De Simone, M., Codella, C., Viti, S., Podio, L., Pineda, J., O'Donoghue, R., Ceccarelli, C., Caselli, P., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Bottinelli, S., Caux, E., Chacón-Tanarro, A., Dulieu, F., Enrique-Romero, J., Fontani, F., Feng, S., Holdship, J., Jiménez-Serra, I., Al-Edhari, A. Jaber, Kahane, C., Lattanzi, V., Oya, Y., Punanova, A., Rimola, A., Sakai, N., Spezzano, S., Sims, I. R., Taquet, V., Testi, L., Theulé, P., Ugliengo, P., Vastel, C., Vasyunin, A. I., Vazart, F., Yamamoto, S., Witzel, A., Schutzer, A. de A., Rivera-Ortiz, P. R., Lefloch, B., Gusdorf, A., Favre, C., Segura-Cox, D., Lopez-Sepulcre, A., Neri, R., Ospina-Zamudio, J., De Simone, M., Codella, C., Viti, S., Podio, L., Pineda, J., O'Donoghue, R., Ceccarelli, C., Caselli, P., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Bottinelli, S., Caux, E., Chacón-Tanarro, A., Dulieu, F., Enrique-Romero, J., Fontani, F., Feng, S., Holdship, J., Jiménez-Serra, I., Al-Edhari, A. Jaber, Kahane, C., Lattanzi, V., Oya, Y., Punanova, A., Rimola, A., Sakai, N., Spezzano, S., Sims, I. R., Taquet, V., Testi, L., Theulé, P., Ugliengo, P., Vastel, C., Vasyunin, A. I., Vazart, F., Yamamoto, S., and Witzel, A.

Abstract

Protostellar jets are an important agent of star formation feedback, tightly connected with the mass-accretion process. The history of jet formation and mass-ejection provides constraints on the mass accretion history and the nature of the driving source. We want to characterize the time-variability of the mass-ejection phenomena at work in the Class 0 protostellar phase, in order to better understand the dynamics of the outflowing gas and bring more constraints on the origin of the jet chemical composition and the mass-accretion history. We have observed the emission of the CO 2-1 and SO N_J=5_4-4_3 rotational transitions with NOEMA, towards the intermediate-mass Class 0 protostellar system Cep E. The CO high-velocity jet emission reveals a central component associated with high-velocity molecular knots, also detected in SO, surrounded by a collimated layer of entrained gas. The gas layer appears to accelerate along the main axis over a length scale delta_0 ~700 au, while its diameter gradually increases up to several 1000au at 2000au from the protostar. The jet is fragmented into 18 knots of mass ~10^-3 Msun, unevenly distributed between the northern and southern lobes, with velocity variations up to 15 km/s close to the protostar, well below the jet terminal velocities. The knot interval distribution is approximately bimodal with a scale of ~50-80yr close to the protostar and ~150-200yr at larger distances >12". The mass-loss rates derived from knot masses are overall steady, with values of 2.7x10^-5 Msun/yr (8.9x10^-6 Msun/yr) in the northern (southern) lobe. The interaction of the ambient protostellar material with high-velocity knots drives the formation of a molecular layer around the jet, which accounts for the higher mass-loss rate in the north. The jet dynamics are well accounted for by a simple precession model with a period of 2000yr and a mass-ejection period of 55yr., Comment: 13 pages, 9 figures, 3 table. Accepted in A&A

Published
2022
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23. The chemical nature of Orion protostars: Are ORANGES different from PEACHES? ORANGES II

Author

Bouvier, M., Ceccarelli, C., López-Sepulcre, A., Sakai, N., Yamamoto, S., Yang, Y. -L., Bouvier, M., Ceccarelli, C., López-Sepulcre, A., Sakai, N., Yamamoto, S., and Yang, Y. -L.

Abstract

Understanding the chemical past of our Sun and how life appeared on Earth is no mean feat. The best strategy we can adopt is to study newborn stars located in an environment similar to the one in which our Sun was born and assess their chemical content. In particular, hot corinos are prime targets since recent studies showed correlations between interstellar Complex Organic Molecules (iCOMs) abundances from hot corinos and comets. The ORion ALMA New GEneration Survey (ORANGES) aims to assess the number of hot corinos in the closest and best analogue to our Sun's birth environment, the OMC-2/3 filament. In this context, we investigated the chemical nature of 19 solar-mass protostars and found that 26\% of our sample sources shows warm methanol emission indicative of hot corinos. Compared to the Perseus low-mass star-forming region, where the PErseus ALMA CHEmistry Survey (PEACHES) detected $\sim 60$\% of hot corinos, the latter seem to be relatively scarce in the OMC-2/3 filament. While this suggests that the chemical nature of protostars in Orion and Perseus is different, improved statistics are needed in order to consolidate this result. If the two regions are truly different, this would indicate that the environment is likely playing a role in shaping the chemical composition of protostars., Comment: 16 pages, 8 figures, Accepted in ApJ

Published
2022
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24. Importance of source structure on complex organics emission. I. Observations of CH$_3$OH from low-mass to high-mass protostars

Author

van Gelder, M. L., Nazari, P., Tabone, B., Ahmadi, A., van Dishoeck, E. F., Beltrán, M. T., Fuller, G. A., Sakai, N., Sánchez-Monge, Á., Schilke, P., Yang, Y. -L., Zhang, Y., van Gelder, M. L., Nazari, P., Tabone, B., Ahmadi, A., van Dishoeck, E. F., Beltrán, M. T., Fuller, G. A., Sakai, N., Sánchez-Monge, Á., Schilke, P., Yang, Y. -L., and Zhang, Y.

Abstract

Complex organic molecules (COMs) are often observed toward embedded Class 0 and I protostars. However, not all Class 0 and I protostars exhibit COMs emission. In this work, variations in methanol (CH$_3$OH) emission are studied to test if absence of CH$_3$OH emission can be linked to source properties. Combining both new and archival observations with ALMA and sources from the literature, a sample of 184 low-mass and high-mass protostars is investigated. The warm (T > 100 K) gaseous CH$_3$OH mass, $M_{\rm CH_3OH}$, is determined for each source using primarily optically thin isotopologues. On average, Class I protostellar systems seem to have less warm $M_{\rm CH_3OH}$ ($<10^{-10}$ M$_\odot$) than younger Class 0 sources ($\sim10^{-7}$ M$_\odot$). High-mass sources in our sample show higher warm $M_{\rm CH_3OH}$ up to $10^{-7}-10^{-3}$ M$_\odot$. To take into account the effect of the source's overall mass on $M_{\rm CH_3OH}$, a normalized CH$_3$OH mass is defined as $M_{\rm CH_3OH}/M_{\rm dust,0}$, where $M_{\rm dust,0}$ is the cold + warm dust mass within a fixed radius. Excluding upper limits, a simple power-law fit to the normalized warm CH$_3$OH masses results in $M_{\rm CH_3OH}/M_{\rm dust,0}\propto L_{\rm bol}^{0.70\pm0.05}$. This is in good agreement with a simple hot core toy model which predicts that the normalized $M_{\rm CH_3OH}$ increases with $L_{\rm bol}^{0.75}$ due to the snowline moving outward. Sources for which the size of the disk is equivalent or smaller than the estimated 100 K radius agree well with the best-fit power-law model, whereas sources with significantly larger disks show up to two orders of magnitude lower normalized warm CH$_3$OH masses. Based on the latter results, we suggest that source structure such as a disk can result in colder gas and thus fewer COMs in the gas phase. Additionally, optically thick dust can hide the emission of COMs., Comment: 22 pages, 6 figures, accepted for publication in A&A

Published
2022
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25. Safety and efficacy of hydrothermal duodenal mucosal resurfacing in patients with type 2 diabetes: The randomised, double-blind, sham-controlled, multicentre REVITA-2 feasibility trial

Author

Mingrone, Geltrude, Van Baar, A. C. G., Deviere, J., Hopkins, D., Moura, E., Cercato, C., Rajagopalan, H., Lopez-Talavera, J. C., White, K., Bhambhani, V., Costamagna, Guido, Haidry, R., Grecco, E., Galvao Neto, M., Aithal, G., Repici, A., Hayee, B., Haji, A., Morris, A. J., Bisschops, R., Chouhan, M. D., Sakai, N. S., Bhatt, D. L., Sanyal, A. J., Bergman, J. J. G. H. M., Mingrone G. (ORCID:0000-0003-2021-528X), Costamagna G. (ORCID:0000-0002-8100-2731), Mingrone, Geltrude, Van Baar, A. C. G., Deviere, J., Hopkins, D., Moura, E., Cercato, C., Rajagopalan, H., Lopez-Talavera, J. C., White, K., Bhambhani, V., Costamagna, Guido, Haidry, R., Grecco, E., Galvao Neto, M., Aithal, G., Repici, A., Hayee, B., Haji, A., Morris, A. J., Bisschops, R., Chouhan, M. D., Sakai, N. S., Bhatt, D. L., Sanyal, A. J., Bergman, J. J. G. H. M., Mingrone G. (ORCID:0000-0003-2021-528X), and Costamagna G. (ORCID:0000-0002-8100-2731)

Abstract

Objective: Hydrothermal duodenal mucosal resurfacing (DMR) is a safe, outpatient endoscopic procedure. REVITA-2, a double-blind, superiority randomised controlled trial, investigates safety and efficacy of DMR using the single catheter Revita system (Revita DMR (catheter and system)), on glycaemic control and liver fat content in type 2 diabetes (T2D). Design: Eligible patients (haemoglobin A1c (HbA1c) 59-86 mmol/mol, body mass index≥24 and ≤40 kg/m2, fasting insulin >48.6 pmol/L, ≥1 oral antidiabetic medication) enrolled in Europe and Brazil. Primary endpoints were safety, change from baseline in HbA1c at 24 weeks, and liver MRI proton-density fat fraction (MRI-PDFF) at 12 weeks. Results: Overall mITT (DMR n=56; sham n=52), 24 weeks post DMR, median (IQR) HbA1c change was -10.4 (18.6) mmol/mol in DMR group versus -7.1 (16.4) mmol/mol in sham group (p=0.147). In patients with baseline liver MRI-PDFF >5% (DMR n=48; sham n=43), 12-week post-DMR liver-fat change was -5.4 (5.6)% in DMR group versus -2.9 (6.2)% in sham group (p=0.096). Results from prespecified interaction testing and clinical parameter assessment showed heterogeneity between European (DMR n=39; sham n=37) and Brazilian (DMR n=17; sham n=16) populations (p=0.063); therefore, results were stratified by region. In European mITT, 24 weeks post DMR, median (IQR) HbA1c change was -6.6 mmol/mol (17.5 mmol/mol) versus -3.3 mmol/mol (10.9 mmol/mol) post-sham (p=0.033); 12-week post-DMR liver-fat change was -5.4% (6.1%) versus -2.2% (4.3%) post-sham (p=0.035). Brazilian mITT results trended towards DMR benefit in HbA1c, but not liver fat, in context of a large sham effect. In overall PP, patients with high baseline fasting plasma glucose ((FPG)≥10 mmol/L) had significantly greater reductions in HbA1c post-DMR versus sham (p=0.002). Most adverse events were mild and transient. Conclusions: DMR is safe and exerts beneficial disease-modifying metabolic effects in T2D with or without non-alcoholic liver disease

Published
2022

26. Global Impact of COVID-19 on Stroke Care and IV Thrombolysis

Author

Nogueira, R.G. Qureshi, M.M. Abdalkader, M. Martins, S.O. Yamagami, H. Qiu, Z. Mansour, O.Y. Sathya, A. Czlonkowska, A. Tsivgoulis, G. Aguiar de Sousa, D. Demeestere, J. Mikulik, R. Vanacker, P. Siegler, J.E. Kõrv, J. Biller, J. Liang, C.W. Sangha, N.S. Zha, A.M. Czap, A.L. Holmstedt, C.A. Turan, T.N. Ntaios, G. Malhotra, K. Tayal, A. Loochtan, A. Ranta, A. Mistry, E.A. Alexandrov, A.W. Huang, D.Y. Yaghi, S. Raz, E. Sheth, S.A. Mohammaden, M.H. Frankel, M. Bila Lamou, E.G. Aref, H.M. Elbassiouny, A. Hassan, F. Menecie, T. Mustafa, W. Shokri, H.M. Roushdy, T. Sarfo, F.S. Alabi, T.O. Arabambi, B. Nwazor, E.O. Sunmonu, T.A. Wahab, K. Yaria, J. Mohammed, H.H. Adebayo, P.B. Riahi, A.D. Sassi, S.B. Gwaunza, L. Ngwende, G.W. Sahakyan, D. Rahman, A. Ai, Z. Bai, F. Duan, Z. Hao, Y. Huang, W. Li, G. Li, W. Liu, G. Luo, J. Shang, X. Sui, Y. Tian, L. Wen, H. Wu, B. Yan, Y. Yuan, Z. Zhang, H. Zhang, J. Zhao, W. Zi, W. Leung, T.W. Chugh, C. Huded, V. Menon, B. Pandian, J.D. Sylaja, P.N. Usman, F.S. Farhoudi, M. Hokmabadi, E.S. Horev, A. Reznik, A. Sivan Hoffmann, R. Ohara, N. Sakai, N. Watanabe, D. Yamamoto, R. Doijiri, R. Tokuda, N. Yamada, T. Terasaki, T. Yazawa, Y. Uwatoko, T. Dembo, T. Shimizu, H. Sugiura, Y. Miyashita, F. Fukuda, H. Miyake, K. Shimbo, J. Sugimura, Y. Yagita, Y. Takenobu, Y. Matsumaru, Y. Yamada, S. Kono, R. Kanamaru, T. Yamazaki, H. Sakaguchi, M. Todo, K. Yamamoto, N. Sonoda, K. Yoshida, T. Hashimoto, H. Nakahara, I. Kondybayeva, A. Faizullina, K. Kamenova, S. Zhanuzakov, M. Baek, J.-H. Hwang, Y. Lee, J.S. Lee, S.B. Moon, J. Park, H. Seo, J.H. Seo, K.-D. Sohn, S.I. Young, C.J. Ahdab, R. Wan Zaidi, W.A. Aziz, Z.A. Basri, H.B. Chung, L.W. Ibrahim, A.B. Ibrahim, K.A. Looi, I. Tan, W.Y. Yahya, N.W. Groppa, S. Leahu, P. Al Hashmi, A.M. Imam, Y.Z. Akhtar, N. Pineda-Franks, M.C. Co, C.O. Kandyba, D. Alhazzani, A. Al-Jehani, H. Tham, C.H. Mamauag, M.J. Venketasubramanian, N. Chen, C.-H. Tang, S.-C. Churojana, A. Akil, E. Aykaç, Ö. Ozdemir, A.O. Giray, S. Hussain, S. and Nogueira, R.G. Qureshi, M.M. Abdalkader, M. Martins, S.O. Yamagami, H. Qiu, Z. Mansour, O.Y. Sathya, A. Czlonkowska, A. Tsivgoulis, G. Aguiar de Sousa, D. Demeestere, J. Mikulik, R. Vanacker, P. Siegler, J.E. Kõrv, J. Biller, J. Liang, C.W. Sangha, N.S. Zha, A.M. Czap, A.L. Holmstedt, C.A. Turan, T.N. Ntaios, G. Malhotra, K. Tayal, A. Loochtan, A. Ranta, A. Mistry, E.A. Alexandrov, A.W. Huang, D.Y. Yaghi, S. Raz, E. Sheth, S.A. Mohammaden, M.H. Frankel, M. Bila Lamou, E.G. Aref, H.M. Elbassiouny, A. Hassan, F. Menecie, T. Mustafa, W. Shokri, H.M. Roushdy, T. Sarfo, F.S. Alabi, T.O. Arabambi, B. Nwazor, E.O. Sunmonu, T.A. Wahab, K. Yaria, J. Mohammed, H.H. Adebayo, P.B. Riahi, A.D. Sassi, S.B. Gwaunza, L. Ngwende, G.W. Sahakyan, D. Rahman, A. Ai, Z. Bai, F. Duan, Z. Hao, Y. Huang, W. Li, G. Li, W. Liu, G. Luo, J. Shang, X. Sui, Y. Tian, L. Wen, H. Wu, B. Yan, Y. Yuan, Z. Zhang, H. Zhang, J. Zhao, W. Zi, W. Leung, T.W. Chugh, C. Huded, V. Menon, B. Pandian, J.D. Sylaja, P.N. Usman, F.S. Farhoudi, M. Hokmabadi, E.S. Horev, A. Reznik, A. Sivan Hoffmann, R. Ohara, N. Sakai, N. Watanabe, D. Yamamoto, R. Doijiri, R. Tokuda, N. Yamada, T. Terasaki, T. Yazawa, Y. Uwatoko, T. Dembo, T. Shimizu, H. Sugiura, Y. Miyashita, F. Fukuda, H. Miyake, K. Shimbo, J. Sugimura, Y. Yagita, Y. Takenobu, Y. Matsumaru, Y. Yamada, S. Kono, R. Kanamaru, T. Yamazaki, H. Sakaguchi, M. Todo, K. Yamamoto, N. Sonoda, K. Yoshida, T. Hashimoto, H. Nakahara, I. Kondybayeva, A. Faizullina, K. Kamenova, S. Zhanuzakov, M. Baek, J.-H. Hwang, Y. Lee, J.S. Lee, S.B. Moon, J. Park, H. Seo, J.H. Seo, K.-D. Sohn, S.I. Young, C.J. Ahdab, R. Wan Zaidi, W.A. Aziz, Z.A. Basri, H.B. Chung, L.W. Ibrahim, A.B. Ibrahim, K.A. Looi, I. Tan, W.Y. Yahya, N.W. Groppa, S. Leahu, P. Al Hashmi, A.M. Imam, Y.Z. Akhtar, N. Pineda-Franks, M.C. Co, C.O. Kandyba, D. Alhazzani, A. Al-Jehani, H. Tham, C.H. Mamauag, M.J. Venketasubramanian, N. Chen, C.-H. Tang, S.-C. Churojana, A. Akil, E. Aykaç, Ö. Ozdemir, A.O. Giray, S. Hussain, S.

Abstract

OBJECTIVE: To measure the global impact of COVID-19 pandemic on volumes of IV thrombolysis (IVT), IVT transfers, and stroke hospitalizations over 4 months at the height of the pandemic (March 1 to June 30, 2020) compared with 2 control 4-month periods. METHODS: We conducted a cross-sectional, observational, retrospective study across 6 continents, 70 countries, and 457 stroke centers. Diagnoses were identified by their ICD-10 codes or classifications in stroke databases. RESULTS: There were 91,373 stroke admissions in the 4 months immediately before compared to 80,894 admissions during the pandemic months, representing an 11.5% (95% confidence interval [CI] -11.7 to -11.3, p < 0.0001) decline. There were 13,334 IVT therapies in the 4 months preceding compared to 11,570 procedures during the pandemic, representing a 13.2% (95% CI -13.8 to -12.7, p < 0.0001) drop. Interfacility IVT transfers decreased from 1,337 to 1,178, or an 11.9% decrease (95% CI -13.7 to -10.3, p = 0.001). Recovery of stroke hospitalization volume (9.5%, 95% CI 9.2-9.8, p < 0.0001) was noted over the 2 later (May, June) vs the 2 earlier (March, April) pandemic months. There was a 1.48% stroke rate across 119,967 COVID-19 hospitalizations. Severe acute respiratory syndrome coronavirus 2 (SARS-CoV-2) infection was noted in 3.3% (1,722/52,026) of all stroke admissions. CONCLUSIONS: The COVID-19 pandemic was associated with a global decline in the volume of stroke hospitalizations, IVT, and interfacility IVT transfers. Primary stroke centers and centers with higher COVID-19 inpatient volumes experienced steeper declines. Recovery of stroke hospitalization was noted in the later pandemic months. © 2021 American Academy of Neurology.

Published
2021

27. Decline in subarachnoid haemorrhage volumes associated with the first wave of the COVID-19 pandemic

Author

Nguyen, T.N. Haussen, D.C. Qureshi, M.M. Yamagami, H. Fujinaka, T. Mansour, O.Y. Abdalkader, M. Frankel, M. Qiu, Z. Taylor, A. Lylyk, P. Eker, O.F. Mechtouff, L. Piotin, M. Lima, F.O. Mont'Alverne, F. Izzath, W. Sakai, N. Mohammaden, M. Al-Bayati, A.R. Renieri, L. Mangiafico, S. Ozretic, D. Chalumeau, V. Ahmad, S. Rashid, U. Hussain, S.I. John, S. Griffin, E. Thornton, J. Fiorot, J.A. Rivera, R. Hammami, N. Cervantes-Arslanian, A.M. Dasenbrock, H.H. Vu, H.L. Nguyen, V.Q. Hetts, S. Bourcier, R. Guile, R. Walker, M. Sharma, M. Frei, D. Jabbour, P. Herial, N. Al-Mufti, F. Ozdemir, A.O. Aykac, O. Gandhi, D. Chugh, C. Matouk, C. Lavoie, P. Edgell, R. Beer-Furlan, A. Chen, M. Killer-Oberpfalzer, M. Pereira, V.M. Nicholson, P. Huded, V. Ohara, N. Watanabe, D. Shin, D.H. Magalhaes, P.S.C. Kikano, R. Ortega-Gutierrez, S. Farooqui, M. Abou-Hamden, A. Amano, T. Yamamoto, R. Weeks, A. Cora, E.A. Sivan-Hoffmann, R. Crosa, R. Möhlenbruch, M. Nagel, S. Al-Jehani, H. Sheth, S.A. Rivera, V.S.L. Siegler, J.E. Sani, A.F. Puri, A.S. Kuhn, A.L. Bernava, G. Machi, P. Abud, D.G. Pontes-Neto, O.M. Wakhloo, A.K. Voetsch, B. Raz, E. Yaghi, S. Mehta, B.P. Kimura, N. Murakami, M. Lee, J.S. Hong, J.M. Fahed, R. Walker, G. Hagashi, E. Cordina, S.M. Roh, H.G. Wong, K. Arenillas, J.F. Martinez-Galdamez, M. Blasco, J. Vasquez, A.R. Fonseca, L. Silva, M.L. Wu, T.Y. John, S. Brehm, A. Psychogios, M. Mack, W.J. Tenser, M. Todaka, T. Fujimura, M. Novakovic, R. Deguchi, J. Sugiura, Y. Tokimura, H. Khatri, R. Kelly, M. Peeling, L. Murayama, Y. Winters, H.S. Wong, J. Teleb, M. Payne, J. Fukuda, H. Miyake, K. Shimbo, J. Sugimura, Y. Uno, M. Takenobu, Y. Matsumaru, Y. Yamada, S. Kono, R. Kanamaru, T. Morimoto, M. Iida, J. Saini, V. Yavagal, D. Bushnaq, S. Huang, W. Linfante, I. Kirmani, J. Liebeskind, D.S. Szeder, V. Shah, R. Devlin, T.G. Birnbaum, L. Luo, J. Churojana, A. Masoud, H.E. Lopez, C.Y. Steinfort, B. Ma, A. Hassan, A.E. Al Hashmi, A. McDermott, M. Mokin, M. Chebl, A. Kargiotis, O. Tsivgoulis and Nguyen, T.N. Haussen, D.C. Qureshi, M.M. Yamagami, H. Fujinaka, T. Mansour, O.Y. Abdalkader, M. Frankel, M. Qiu, Z. Taylor, A. Lylyk, P. Eker, O.F. Mechtouff, L. Piotin, M. Lima, F.O. Mont'Alverne, F. Izzath, W. Sakai, N. Mohammaden, M. Al-Bayati, A.R. Renieri, L. Mangiafico, S. Ozretic, D. Chalumeau, V. Ahmad, S. Rashid, U. Hussain, S.I. John, S. Griffin, E. Thornton, J. Fiorot, J.A. Rivera, R. Hammami, N. Cervantes-Arslanian, A.M. Dasenbrock, H.H. Vu, H.L. Nguyen, V.Q. Hetts, S. Bourcier, R. Guile, R. Walker, M. Sharma, M. Frei, D. Jabbour, P. Herial, N. Al-Mufti, F. Ozdemir, A.O. Aykac, O. Gandhi, D. Chugh, C. Matouk, C. Lavoie, P. Edgell, R. Beer-Furlan, A. Chen, M. Killer-Oberpfalzer, M. Pereira, V.M. Nicholson, P. Huded, V. Ohara, N. Watanabe, D. Shin, D.H. Magalhaes, P.S.C. Kikano, R. Ortega-Gutierrez, S. Farooqui, M. Abou-Hamden, A. Amano, T. Yamamoto, R. Weeks, A. Cora, E.A. Sivan-Hoffmann, R. Crosa, R. Möhlenbruch, M. Nagel, S. Al-Jehani, H. Sheth, S.A. Rivera, V.S.L. Siegler, J.E. Sani, A.F. Puri, A.S. Kuhn, A.L. Bernava, G. Machi, P. Abud, D.G. Pontes-Neto, O.M. Wakhloo, A.K. Voetsch, B. Raz, E. Yaghi, S. Mehta, B.P. Kimura, N. Murakami, M. Lee, J.S. Hong, J.M. Fahed, R. Walker, G. Hagashi, E. Cordina, S.M. Roh, H.G. Wong, K. Arenillas, J.F. Martinez-Galdamez, M. Blasco, J. Vasquez, A.R. Fonseca, L. Silva, M.L. Wu, T.Y. John, S. Brehm, A. Psychogios, M. Mack, W.J. Tenser, M. Todaka, T. Fujimura, M. Novakovic, R. Deguchi, J. Sugiura, Y. Tokimura, H. Khatri, R. Kelly, M. Peeling, L. Murayama, Y. Winters, H.S. Wong, J. Teleb, M. Payne, J. Fukuda, H. Miyake, K. Shimbo, J. Sugimura, Y. Uno, M. Takenobu, Y. Matsumaru, Y. Yamada, S. Kono, R. Kanamaru, T. Morimoto, M. Iida, J. Saini, V. Yavagal, D. Bushnaq, S. Huang, W. Linfante, I. Kirmani, J. Liebeskind, D.S. Szeder, V. Shah, R. Devlin, T.G. Birnbaum, L. Luo, J. Churojana, A. Masoud, H.E. Lopez, C.Y. Steinfort, B. Ma, A. Hassan, A.E. Al Hashmi, A. McDermott, M. Mokin, M. Chebl, A. Kargiotis, O. Tsivgoulis

Abstract

Background During the COVID-19 pandemic, decreased volumes of stroke admissions and mechanical thrombectomy were reported. The study's objective was to examine whether subarachnoid haemorrhage (SAH) hospitalisations and ruptured aneurysm coiling interventions demonstrated similar declines. Methods We conducted a cross-sectional, retrospective, observational study across 6 continents, 37 countries and 140 comprehensive stroke centres. Patients with the diagnosis of SAH, aneurysmal SAH, ruptured aneurysm coiling interventions and COVID-19 were identified by prospective aneurysm databases or by International Classification of Diseases, 10th Revision, codes. The 3-month cumulative volume, monthly volumes for SAH hospitalisations and ruptured aneurysm coiling procedures were compared for the period before (1 year and immediately before) and during the pandemic, defined as 1 March-31 May 2020. The prior 1-year control period (1 March-31 May 2019) was obtained to account for seasonal variation. Findings There was a significant decline in SAH hospitalisations, with 2044 admissions in the 3 months immediately before and 1585 admissions during the pandemic, representing a relative decline of 22.5% (95% CI -24.3% to -20.7%, p<0.0001). Embolisation of ruptured aneurysms declined with 1170-1035 procedures, respectively, representing an 11.5% (95%CI -13.5% to -9.8%, p=0.002) relative drop. Subgroup analysis was noted for aneurysmal SAH hospitalisation decline from 834 to 626 hospitalisations, a 24.9% relative decline (95% CI -28.0% to -22.1%, p<0.0001). A relative increase in ruptured aneurysm coiling was noted in low coiling volume hospitals of 41.1% (95% CI 32.3% to 50.6%, p=0.008) despite a decrease in SAH admissions in this tertile. Interpretation There was a relative decrease in the volume of SAH hospitalisations, aneurysmal SAH hospitalisations and ruptured aneurysm embolisations during the COVID-19 pandemic. These findings in SAH are consistent with a decrease i

Published
2021

28. Global impact of COVID-19 on stroke care

Author

Nogueira, R.G. Abdalkader, M. Qureshi, M.M. Frankel, M.R. Mansour, O.Y. Yamagami, H. Qiu, Z. Farhoudi, M. Siegler, J.E. Yaghi, S. Raz, E. Sakai, N. Ohara, N. Piotin, M. Mechtouff, L. Eker, O. Chalumeau, V. Kleinig, T.J. Pop, R. Liu, J. Winters, H.S. Shang, X. Vasquez, A.R. Blasco, J. Arenillas, J.F. Martinez-Galdamez, M. Brehm, A. Psychogios, M.-N. Lylyk, P. Haussen, D.C. Al-Bayati, A.R. Mohammaden, M.H. Fonseca, L. Luís Silva, M. Montalverne, F. Renieri, L. Mangiafico, S. Fischer, U. Gralla, J. Frei, D. Chugh, C. Mehta, B.P. Nagel, S. Mohlenbruch, M. Ortega-Gutierrez, S. Farooqui, M. Hassan, A.E. Taylor, A. Lapergue, B. Consoli, A. Campbell, B.C.V. Sharma, M. Walker, M. Van Horn, N. Fiehler, J. Nguyen, H.T. Nguyen, Q.T. Watanabe, D. Zhang, H. Le, H.V. Nguyen, V.Q. Shah, R. Devlin, T. Khandelwal, P. Linfante, I. Izzath, W. Lavados, P.M. Olavarría, V.V. Sampaio Silva, G. de Carvalho Sousa, A.V. Kirmani, J. Bendszus, M. Amano, T. Yamamoto, R. Doijiri, R. Tokuda, N. Yamada, T. Terasaki, T. Yazawa, Y. Morris, J.G. Griffin, E. Thornton, J. Lavoie, P. Matouk, C. Hill, M.D. Demchuk, A.M. Killer-Oberpfalzer, M. Nahab, F. Altschul, D. Ramos-Pachón, A. Pérez de la Ossa, N. Kikano, R. Boisseau, W. Walker, G. Cordina, S.M. Puri, A. Luisa Kuhn, A. Gandhi, D. Ramakrishnan, P. Novakovic-White, R. Chebl, A. Kargiotis, O. Czap, A. Zha, A. Masoud, H.E. Lopez, C. Ozretic, D. Al-Mufti, F. Zie, W. Duan, Z. Yuan, Z. Huang, W. Hao, Y. Luo, J. Kalousek, V. Bourcier, R. Guile, R. Hetts, S. Al-Jehani, H.M. AlHazzani, A. Sadeghi-Hokmabadi, E. Teleb, M. Payne, J. Lee, J.S. Hong, J.M. Sohn, S.-I. Hwang, Y.-H. Shin, D.H. Roh, H.G. Edgell, R. Khatri, R. Smith, A. Malik, A. Liebeskind, D. Herial, N. Jabbour, P. Magalhaes, P. Ozdemir, A.O. Aykac, O. Uwatoko, T. Dembo, T. Shimizu, H. Sugiura, Y. Miyashita, F. Fukuda, H. Miyake, K. Shimbo, J. Sugimura, Y. Beer-Furlan, A. Joshi, K. Catanese, L. Abud, D.G. Neto, O.G. Mehrpour, M. Al Hashmi, A. Saqqur, M. Mostafa, A. Fifi, J.T. Hussain, S. John, S. Gupt and Nogueira, R.G. Abdalkader, M. Qureshi, M.M. Frankel, M.R. Mansour, O.Y. Yamagami, H. Qiu, Z. Farhoudi, M. Siegler, J.E. Yaghi, S. Raz, E. Sakai, N. Ohara, N. Piotin, M. Mechtouff, L. Eker, O. Chalumeau, V. Kleinig, T.J. Pop, R. Liu, J. Winters, H.S. Shang, X. Vasquez, A.R. Blasco, J. Arenillas, J.F. Martinez-Galdamez, M. Brehm, A. Psychogios, M.-N. Lylyk, P. Haussen, D.C. Al-Bayati, A.R. Mohammaden, M.H. Fonseca, L. Luís Silva, M. Montalverne, F. Renieri, L. Mangiafico, S. Fischer, U. Gralla, J. Frei, D. Chugh, C. Mehta, B.P. Nagel, S. Mohlenbruch, M. Ortega-Gutierrez, S. Farooqui, M. Hassan, A.E. Taylor, A. Lapergue, B. Consoli, A. Campbell, B.C.V. Sharma, M. Walker, M. Van Horn, N. Fiehler, J. Nguyen, H.T. Nguyen, Q.T. Watanabe, D. Zhang, H. Le, H.V. Nguyen, V.Q. Shah, R. Devlin, T. Khandelwal, P. Linfante, I. Izzath, W. Lavados, P.M. Olavarría, V.V. Sampaio Silva, G. de Carvalho Sousa, A.V. Kirmani, J. Bendszus, M. Amano, T. Yamamoto, R. Doijiri, R. Tokuda, N. Yamada, T. Terasaki, T. Yazawa, Y. Morris, J.G. Griffin, E. Thornton, J. Lavoie, P. Matouk, C. Hill, M.D. Demchuk, A.M. Killer-Oberpfalzer, M. Nahab, F. Altschul, D. Ramos-Pachón, A. Pérez de la Ossa, N. Kikano, R. Boisseau, W. Walker, G. Cordina, S.M. Puri, A. Luisa Kuhn, A. Gandhi, D. Ramakrishnan, P. Novakovic-White, R. Chebl, A. Kargiotis, O. Czap, A. Zha, A. Masoud, H.E. Lopez, C. Ozretic, D. Al-Mufti, F. Zie, W. Duan, Z. Yuan, Z. Huang, W. Hao, Y. Luo, J. Kalousek, V. Bourcier, R. Guile, R. Hetts, S. Al-Jehani, H.M. AlHazzani, A. Sadeghi-Hokmabadi, E. Teleb, M. Payne, J. Lee, J.S. Hong, J.M. Sohn, S.-I. Hwang, Y.-H. Shin, D.H. Roh, H.G. Edgell, R. Khatri, R. Smith, A. Malik, A. Liebeskind, D. Herial, N. Jabbour, P. Magalhaes, P. Ozdemir, A.O. Aykac, O. Uwatoko, T. Dembo, T. Shimizu, H. Sugiura, Y. Miyashita, F. Fukuda, H. Miyake, K. Shimbo, J. Sugimura, Y. Beer-Furlan, A. Joshi, K. Catanese, L. Abud, D.G. Neto, O.G. Mehrpour, M. Al Hashmi, A. Saqqur, M. Mostafa, A. Fifi, J.T. Hussain, S. John, S. Gupt

Abstract

Background: The COVID-19 pandemic led to profound changes in the organization of health care systems worldwide. Aims: We sought to measure the global impact of the COVID-19 pandemic on the volumes for mechanical thrombectomy, stroke, and intracranial hemorrhage hospitalizations over a three-month period at the height of the pandemic (1 March–31 May 2020) compared with two control three-month periods (immediately preceding and one year prior). Methods: Retrospective, observational, international study, across 6 continents, 40 countries, and 187 comprehensive stroke centers. The diagnoses were identified by their ICD-10 codes and/or classifications in stroke databases at participating centers. Results: The hospitalization volumes for any stroke, intracranial hemorrhage, and mechanical thrombectomy were 26,699, 4002, and 5191 in the three months immediately before versus 21,576, 3540, and 4533 during the first three pandemic months, representing declines of 19.2% (95%CI, −19.7 to −18.7), 11.5% (95%CI, −12.6 to −10.6), and 12.7% (95%CI, −13.6 to −11.8), respectively. The decreases were noted across centers with high, mid, and low COVID-19 hospitalization burden, and also across high, mid, and low volume stroke/mechanical thrombectomy centers. High-volume COVID-19 centers (−20.5%) had greater declines in mechanical thrombectomy volumes than mid- (−10.1%) and low-volume (−8.7%) centers (p < 0.0001). There was a 1.5% stroke rate across 54,366 COVID-19 hospitalizations. SARS-CoV-2 infection was noted in 3.9% (784/20,250) of all stroke admissions. Conclusion: The COVID-19 pandemic was associated with a global decline in the volume of overall stroke hospitalizations, mechanical thrombectomy procedures, and intracranial hemorrhage admission volumes. Despite geographic variations, these volume reductions were observed regardless of COVID-19 hospitalization burden and pre-pandemic stroke/mechanical thrombectomy volumes. © 2021 World Stroke Organization.

Published
2021

29. Broadband Multi-wavelength Properties of M87 during the 2017 Event Horizon Telescope Campaign

Author

Algaba, J. C., Anczarski, J., Asada, K., Baloković, M., Chandra, S., Cui, Y. -Z, Falcone, A. D., Giroletti, M., Goddi, C., Hada, K., Haggard, D., Jorstad, S., Kaur, A., Kawashima, T., Keating, G., Kim, J. -Y, Kino, M., Komossa, S., Kravchenko, E. V., Krichbaum, T. P., Lee, S. -S, Lu, R. -S, Lucchini, M., Markoff, S., Neilsen, J., Nowak, M. A., Park, J., Principe, G., Ramakrishnan, V., Reynolds, M. T., Sasada, M., Savchenko, S. S., Williamson, K. E., Akiyama, K., Alberdi, A., Alef, W., Anantua, R., Azulay, R., Baczko, A. -K, Ball, D., Barrett, J., Bintley, D., Benson, B. A., Blackburn, L., Blundell, R., Boland, W., Bouman, K. L., Bower, G. C., Boyce, H., Bremer, M., Brinkerink, C. D., Brissenden, R., Britzen, S., Broderick, A. E., Broguiere, D., Bronzwaer, T., Byun, D. -Y, Carlstrom, J. E., Chael, A., Chan, C. -K, Chatterjee, S., Chatterjee, K., Chen, M. -T, Chen, Y., Chesler, P. M., Cho, I., Christian, P., Conway, J. E., Cordes, J. M., Crawford, T. M., Crew, G. B., Cruz-Osorio, A., Davelaar, J., De Laurentis, M., Deane, R., Dempsey, J., Desvignes, G., Dexter, J., Doeleman, S. S., Eatough, R. P., Falcke, H., Farah, J., Fish, V. L., Fomalont, E., Ford, H. A., Fraga-Encinas, R., Friberg, P., Fromm, C. M., Fuentes, A., Galison, P., Gammie, C. F., García, R., Gentaz, O., Georgiev, B., Gold, R., Gómez, J. L., Gómez-Ruiz, A. I., Gu, M., Gurwell, M., Hecht, M. H., Hesper, R., Ho, L. C., Ho, P., Honma, M., Huang, C. -WL., Huang, L., Hughes, D. H., Ikeda, S., Inoue, M., Issaoun, S., James, D. J., Jannuzi, B. T., Janssen, M., Jeter, B., Jiang, W., Jiménez-Rosales, A., Johnson, M. D., Jung, T., Karami, M., Karuppusamy, R., Kettenis, M., Kim, D. -J, Kim, J., Koay, J. Y., Kofuji, Y., Koch, P. M., Koyama, S., Kramer, M., Kramer, C., Kuo, C. -Y, Lauer, T. R., Levis, A., Li, Y. -R, Li, Z., Lindqvist, M., Lico, R., Lindahl, G., Liu, J., Liu, K., Liuzzo, E., Lo, W. -P, Lobanov, A. P., Loinard, L., Lonsdale, C., Macdonald, N. R., Mao, J., Marchili, N., Marrone, D. P., Marscher, A. P., Martí-Vidal, I., Matsushita, S., Matthews, L. D., Medeiros, L., Menten, K. M., Mizuno, I., Mizuno, Y., Moran, J. M., Moriyama, K., Moscibrodzka, M., MÃŒller, C., Musoke, G., Mejías, A. M., Nagai, H., Nagar, N. M., Nakamura, M., Narayan, R., Narayanan, G., Natarajan, I., Nathanail, A., Neri, R., Ni, C., Noutsos, A., Okino, H., Olivares, H., Ortiz-León, G. N., Oyama, T., Ozel, F., Palumbo, D. C. M., Patel, N., Pen, U. -L, Pesce, D. W., Piétu, V., Plambeck, R., Popstefanija, A., Porth, O., Pötzl, F. M., Prather, B., Preciado-López, J. A., Psaltis, D., Pu, H. -Y, Rao, R., Rawlings, M. G., Raymond, A. W., Rezzolla, L., Ricarte, A., Ripperda, B., Roelofs, F., Rogers, A., Ros, E., Rose, M., Roshanineshat, A., Rottmann, H., Roy, A. L., Ruszczyk, C., Rygl, K. L. J., Sánchez, S., Sánchez-Arguelles, D., Savolainen, T., Schloerb, F. P., Schuster, K. -F, Shao, L., Shen, Z., Small, D., Sohn, B. W., Soohoo, J., Sun, H., Tazaki, F., Tetarenko, A. J., Tiede, P., Tilanus, R. P. J., Titus, M., Toma, K., Torne, P., Trent, T., Traianou, E., Trippe, S., Van Bemmel, I., Van Langevelde, H. J., Van Rossum, D. R., Wagner, J., Ward-Thompson, D., Wardle, J., Weintroub, J., Wex, N., Wharton, R., Wielgus, M., Wong, G. N., Wu, Q., Yoon, D., Young, A., Young, K., Younsi, Z., Yuan, F., Yuan, Y. -F, Zensus, J. A., Zhao, G. -Y, Zhao, S. -S, D’Ammando, F., Orienti, M., Abdalla, H., Adam, R., Aharonian, F., Benkhali, F. A., AngÃŒner, E. O., Arcaro, C., Armand, C., Armstrong, T., Ashkar, H., Backes, M., Baghmanyan, V., Barbosa Martins, V., Barnacka, A., Barnard, M., Becherini, Yvonne, Berge, D., Bernlöhr, K., Bi, B., Böttcher, M., Boisson, C., Bolmont, J., De Bony De Lavergne, M., Breuhaus, M., Brun, F., Brun, P., Bryan, M., BÃŒchele, M., Bulik, T., Bylund, Tomas, Caroff, S., Carosi, A., Casanova, S., Chand, T., Chen, A., Cotter, G., CuryÅ‚o, M., Damascene Mbarubucyeye, J., Davids, I. D., Davies, J., Deil, C., Devin, J., Dewilt, P., Dirson, L., Djannati-Ataï, A., Dmytriiev, A., Donath, A., Doroshenko, V., Duffy, C., Dyks, J., Egberts, K., Eichhorn, F., Einecke, S., Emery, G., Ernenwein, J. -P, Feijen, K., Fegan, S., Fiasson, A., De Clairfontaine, G. F., Fontaine, G., Funk, S., FÌßling, M., Gabici, S., Gallant, Y. A., Giavitto, G., Giunti, L., Glawion, D., Glicenstein, J. F., Gottschall, D., Grondin, M. -H, Hahn, J., Haupt, M., Hermann, G., Hinton, J. A., Hofmann, W., Hoischen, C., Holch, T. L., Holler, M., Hörbe, M., Horns, D., Huber, D., Jamrozy, M., Jankowsky, D., Jankowsky, F., Jardin-Blicq, A., Joshi, V., Jung-Richardt, I., Kasai, E., Kastendieck, M. A., KatarzyÅ„ski, K., Katz, U., Khangulyan, D., Khélifi, B., Klepser, S., Kluźniak, W., Komin, N., Konno, R., Kosack, K., Kostunin, D., Kreter, M., Lamanna, G., Lemiere, A., Lemoine-Goumard, M., Lenain, J. -P, Levy, C., Lohse, T., Lypova, I., Mackey, J., Majumdar, J., Malyshev, D., Marandon, V., Marchegiani, P., Marcowith, A., Mares, A., Martí-Devesa, G., Marx, R., Maurin, G., Meintjes, P. J., Meyer, M., Moderski, R., Mohamed, M., Mohrmann, L., Montanari, A., Moore, C., Morris, P., Moulin, E., Muller, J., Murach, T., Nakashima, K., Nayerhoda, A., De Naurois, M., Ndiyavala, H., Niederwanger, F., Niemiec, J., Oakes, L., O’Brien, P., Odaka, H., Ohm, S., Olivera-Nieto, L., De Ona Wilhelmi, E., Ostrowski, M., Panter, M., Panny, S., Parsons, R. D., Peron, G., Peyaud, B., Piel, Q., Pita, S., Poireau, V., Noel, A. P., Prokhorov, D. A., Prokoph, H., PÃŒhlhofer, G., Punch, Michael, Quirrenbach, A., Rauth, R., Reichherzer, P., Reimer, A., Reimer, O., Remy, Q., Renaud, M., Rieger, F., Rinchiuso, L., Romoli, C., Rowell, G., Rudak, B., Ruiz-Velasco, E., Sahakian, V., Sailer, S., Sanchez, D. A., Santangelo, A., Sasaki, M., Scalici, M., Schutte, H. M., Schwanke, U., Schwemmer, S., Seglar-Arroyo, M., Senniappan, M., Seyffert, A. S., Shafi, N., Shiningayamwe, K., Simoni, R., Sinha, A., Sol, H., Specovius, A., Spencer, S., Spir-Jacob, M., Stawarz, Ł., Sun, L., Steenkamp, R., Stegmann, C., Steinmassl, S., Steppa, C., Takahashi, T., Tavernier, T., Taylor, A. M., Terrier, R., Tiziani, D., Tluczykont, M., Tomankova, L., Trichard, C., Tsirou, M., Tuffs, R., Uchiyama, Y., Van Der Walt, D. J., Van Eldik, C., Van Rensburg, C., Van Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Vincent, P., Vink, J., Völk, H. J., Vuillaume, T., Wadiasingh, Z., Wagner, S. J., Watson, J., Werner, F., White, R., Wierzcholska, A., Wong, Y. W., Yusafzai, A., Zacharias, M., Zanin, R., Zargaryan, D., Zdziarski, A. A., Zech, A., Zhu, S. J., Zorn, J., Zouari, S., Å»ywucka, N., Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. A., Artero, M., Asano, K., Baack, D., Babić, A., Baquero, A., De Almeida, U. B., Barrio, J. A., Becerra González, J., Bednarek, W., Bellizzi, L., Bernardini, E., Bernardos, M., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., BoÅ¡njak, Åœ., Busetto, G., Carosi, R., Ceribella, G., Cerruti, M., Chai, Y., Chilingarian, A., Cikota, S., Colak, S. M., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D’Amico, G., D’Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Delgado Mendez, C., Depaoli, D., Di Pierro, F., Di Venere, L., Do Souto Espineira, E., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Ferrara, G., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., García López, R. J., Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Gliwny, P., Godinović, N., Green, J. G., Green, D., Hadasch, D., Hahn, A., Heckmann, L., Herrera, J., Hoang, J., Hrupec, D., HÃŒtten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jiménez, I., Jormanainen, J., Jouvin, L., Kajiwara, Y., Karjalainen, M., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López-Coto, R., López-Moya, M., López-Oramas, A., Loporchio, S., Machado De Oliveira Fraga, B., Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Menchiari, S., Mender, S., Mićanović, S., Miceli, D., Miener, T., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Neustroev, V., Nigro, C., Nilsson, K., Nishijima, K., Noda, K., Nozaki, S., Ohtani, Y., Oka, T., Otero-Santos, J., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pavletić, L., Penil, P., Perennes, C., Persic, M., Moroni, P. G. P., Prandini, E., Priyadarshi, C., Puljak, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Saturni, F. G., Schleicher, B., Schmidt, K., Schweizer, T., Sitarek, J., Å nidarić, I., Sobczynska, D., Spolon, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Surić, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Tosti, L., Truzzi, S., Tutone, A., Ubach, S., Van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Ventura, S., Verguilov, V., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Wunderlich, C., Zarić, D., Adams, C. B., Benbow, W., Brill, A., Capasso, M., Christiansen, J. L., Chromey, A. J., Daniel, M. K., Errando, M., Farrell, K. A., Feng, Q., Finley, J. P., Fortson, L., Furniss, A., Gent, A., Giuri, C., Hassan, T., Hervet, O., Holder, J., Hughes, G., Humensky, T. B., Jin, W., Kaaret, P., Kertzman, M., Kieda, D., Kumar, S., Lang, M. J., Lundy, M., Maier, G., Moriarty, P., Mukherjee, R., Nieto, D., Nievas-Rosillo, M., O’Brien, S., Ong, R. A., Otte, A. N., Patel, S., Pfrang, K., Pohl, M., Prado, R. R., Pueschel, E., Quinn, J., Ragan, K., Reynolds, P. T., Ribeiro, D., Richards, G. T., Roache, E., Rulten, C., Ryan, J. L., Santander, M., Sembroski, G. H., Shang, R., Weinstein, A., Williams, D. A., Williamson, T. J., Hirota, T., Cui, L., Niinuma, K., Ro, H., Sakai, N., Sawada-Satoh, S., Wajima, K., Wang, N., Liu, X., Yonekura, Y., Algaba, J. C., Anczarski, J., Asada, K., Baloković, M., Chandra, S., Cui, Y. -Z, Falcone, A. D., Giroletti, M., Goddi, C., Hada, K., Haggard, D., Jorstad, S., Kaur, A., Kawashima, T., Keating, G., Kim, J. -Y, Kino, M., Komossa, S., Kravchenko, E. V., Krichbaum, T. P., Lee, S. -S, Lu, R. -S, Lucchini, M., Markoff, S., Neilsen, J., Nowak, M. A., Park, J., Principe, G., Ramakrishnan, V., Reynolds, M. T., Sasada, M., Savchenko, S. S., Williamson, K. E., Akiyama, K., Alberdi, A., Alef, W., Anantua, R., Azulay, R., Baczko, A. -K, Ball, D., Barrett, J., Bintley, D., Benson, B. A., Blackburn, L., Blundell, R., Boland, W., Bouman, K. L., Bower, G. C., Boyce, H., Bremer, M., Brinkerink, C. D., Brissenden, R., Britzen, S., Broderick, A. E., Broguiere, D., Bronzwaer, T., Byun, D. -Y, Carlstrom, J. E., Chael, A., Chan, C. -K, Chatterjee, S., Chatterjee, K., Chen, M. -T, Chen, Y., Chesler, P. M., Cho, I., Christian, P., Conway, J. E., Cordes, J. M., Crawford, T. M., Crew, G. B., Cruz-Osorio, A., Davelaar, J., De Laurentis, M., Deane, R., Dempsey, J., Desvignes, G., Dexter, J., Doeleman, S. S., Eatough, R. P., Falcke, H., Farah, J., Fish, V. L., Fomalont, E., Ford, H. A., Fraga-Encinas, R., Friberg, P., Fromm, C. M., Fuentes, A., Galison, P., Gammie, C. F., García, R., Gentaz, O., Georgiev, B., Gold, R., Gómez, J. L., Gómez-Ruiz, A. I., Gu, M., Gurwell, M., Hecht, M. H., Hesper, R., Ho, L. C., Ho, P., Honma, M., Huang, C. -WL., Huang, L., Hughes, D. H., Ikeda, S., Inoue, M., Issaoun, S., James, D. J., Jannuzi, B. T., Janssen, M., Jeter, B., Jiang, W., Jiménez-Rosales, A., Johnson, M. D., Jung, T., Karami, M., Karuppusamy, R., Kettenis, M., Kim, D. -J, Kim, J., Koay, J. Y., Kofuji, Y., Koch, P. M., Koyama, S., Kramer, M., Kramer, C., Kuo, C. -Y, Lauer, T. R., Levis, A., Li, Y. -R, Li, Z., Lindqvist, M., Lico, R., Lindahl, G., Liu, J., Liu, K., Liuzzo, E., Lo, W. -P, Lobanov, A. P., Loinard, L., Lonsdale, C., Macdonald, N. R., Mao, J., Marchili, N., Marrone, D. P., Marscher, A. P., Martí-Vidal, I., Matsushita, S., Matthews, L. D., Medeiros, L., Menten, K. M., Mizuno, I., Mizuno, Y., Moran, J. M., Moriyama, K., Moscibrodzka, M., MÃŒller, C., Musoke, G., Mejías, A. M., Nagai, H., Nagar, N. M., Nakamura, M., Narayan, R., Narayanan, G., Natarajan, I., Nathanail, A., Neri, R., Ni, C., Noutsos, A., Okino, H., Olivares, H., Ortiz-León, G. N., Oyama, T., Ozel, F., Palumbo, D. C. M., Patel, N., Pen, U. -L, Pesce, D. W., Piétu, V., Plambeck, R., Popstefanija, A., Porth, O., Pötzl, F. M., Prather, B., Preciado-López, J. A., Psaltis, D., Pu, H. -Y, Rao, R., Rawlings, M. G., Raymond, A. W., Rezzolla, L., Ricarte, A., Ripperda, B., Roelofs, F., Rogers, A., Ros, E., Rose, M., Roshanineshat, A., Rottmann, H., Roy, A. L., Ruszczyk, C., Rygl, K. L. J., Sánchez, S., Sánchez-Arguelles, D., Savolainen, T., Schloerb, F. P., Schuster, K. -F, Shao, L., Shen, Z., Small, D., Sohn, B. W., Soohoo, J., Sun, H., Tazaki, F., Tetarenko, A. J., Tiede, P., Tilanus, R. P. J., Titus, M., Toma, K., Torne, P., Trent, T., Traianou, E., Trippe, S., Van Bemmel, I., Van Langevelde, H. J., Van Rossum, D. R., Wagner, J., Ward-Thompson, D., Wardle, J., Weintroub, J., Wex, N., Wharton, R., Wielgus, M., Wong, G. N., Wu, Q., Yoon, D., Young, A., Young, K., Younsi, Z., Yuan, F., Yuan, Y. -F, Zensus, J. A., Zhao, G. -Y, Zhao, S. -S, D’Ammando, F., Orienti, M., Abdalla, H., Adam, R., Aharonian, F., Benkhali, F. A., AngÃŒner, E. O., Arcaro, C., Armand, C., Armstrong, T., Ashkar, H., Backes, M., Baghmanyan, V., Barbosa Martins, V., Barnacka, A., Barnard, M., Becherini, Yvonne, Berge, D., Bernlöhr, K., Bi, B., Böttcher, M., Boisson, C., Bolmont, J., De Bony De Lavergne, M., Breuhaus, M., Brun, F., Brun, P., Bryan, M., BÃŒchele, M., Bulik, T., Bylund, Tomas, Caroff, S., Carosi, A., Casanova, S., Chand, T., Chen, A., Cotter, G., CuryÅ‚o, M., Damascene Mbarubucyeye, J., Davids, I. D., Davies, J., Deil, C., Devin, J., Dewilt, P., Dirson, L., Djannati-Ataï, A., Dmytriiev, A., Donath, A., Doroshenko, V., Duffy, C., Dyks, J., Egberts, K., Eichhorn, F., Einecke, S., Emery, G., Ernenwein, J. -P, Feijen, K., Fegan, S., Fiasson, A., De Clairfontaine, G. F., Fontaine, G., Funk, S., FÌßling, M., Gabici, S., Gallant, Y. A., Giavitto, G., Giunti, L., Glawion, D., Glicenstein, J. F., Gottschall, D., Grondin, M. -H, Hahn, J., Haupt, M., Hermann, G., Hinton, J. A., Hofmann, W., Hoischen, C., Holch, T. L., Holler, M., Hörbe, M., Horns, D., Huber, D., Jamrozy, M., Jankowsky, D., Jankowsky, F., Jardin-Blicq, A., Joshi, V., Jung-Richardt, I., Kasai, E., Kastendieck, M. A., KatarzyÅ„ski, K., Katz, U., Khangulyan, D., Khélifi, B., Klepser, S., Kluźniak, W., Komin, N., Konno, R., Kosack, K., Kostunin, D., Kreter, M., Lamanna, G., Lemiere, A., Lemoine-Goumard, M., Lenain, J. -P, Levy, C., Lohse, T., Lypova, I., Mackey, J., Majumdar, J., Malyshev, D., Marandon, V., Marchegiani, P., Marcowith, A., Mares, A., Martí-Devesa, G., Marx, R., Maurin, G., Meintjes, P. J., Meyer, M., Moderski, R., Mohamed, M., Mohrmann, L., Montanari, A., Moore, C., Morris, P., Moulin, E., Muller, J., Murach, T., Nakashima, K., Nayerhoda, A., De Naurois, M., Ndiyavala, H., Niederwanger, F., Niemiec, J., Oakes, L., O’Brien, P., Odaka, H., Ohm, S., Olivera-Nieto, L., De Ona Wilhelmi, E., Ostrowski, M., Panter, M., Panny, S., Parsons, R. D., Peron, G., Peyaud, B., Piel, Q., Pita, S., Poireau, V., Noel, A. P., Prokhorov, D. A., Prokoph, H., PÃŒhlhofer, G., Punch, Michael, Quirrenbach, A., Rauth, R., Reichherzer, P., Reimer, A., Reimer, O., Remy, Q., Renaud, M., Rieger, F., Rinchiuso, L., Romoli, C., Rowell, G., Rudak, B., Ruiz-Velasco, E., Sahakian, V., Sailer, S., Sanchez, D. A., Santangelo, A., Sasaki, M., Scalici, M., Schutte, H. M., Schwanke, U., Schwemmer, S., Seglar-Arroyo, M., Senniappan, M., Seyffert, A. S., Shafi, N., Shiningayamwe, K., Simoni, R., Sinha, A., Sol, H., Specovius, A., Spencer, S., Spir-Jacob, M., Stawarz, Ł., Sun, L., Steenkamp, R., Stegmann, C., Steinmassl, S., Steppa, C., Takahashi, T., Tavernier, T., Taylor, A. M., Terrier, R., Tiziani, D., Tluczykont, M., Tomankova, L., Trichard, C., Tsirou, M., Tuffs, R., Uchiyama, Y., Van Der Walt, D. J., Van Eldik, C., Van Rensburg, C., Van Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Vincent, P., Vink, J., Völk, H. J., Vuillaume, T., Wadiasingh, Z., Wagner, S. J., Watson, J., Werner, F., White, R., Wierzcholska, A., Wong, Y. W., Yusafzai, A., Zacharias, M., Zanin, R., Zargaryan, D., Zdziarski, A. A., Zech, A., Zhu, S. J., Zorn, J., Zouari, S., Å»ywucka, N., Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. A., Artero, M., Asano, K., Baack, D., Babić, A., Baquero, A., De Almeida, U. B., Barrio, J. A., Becerra González, J., Bednarek, W., Bellizzi, L., Bernardini, E., Bernardos, M., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., BoÅ¡njak, Åœ., Busetto, G., Carosi, R., Ceribella, G., Cerruti, M., Chai, Y., Chilingarian, A., Cikota, S., Colak, S. M., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D’Amico, G., D’Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Delgado Mendez, C., Depaoli, D., Di Pierro, F., Di Venere, L., Do Souto Espineira, E., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Ferrara, G., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., García López, R. J., Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Gliwny, P., Godinović, N., Green, J. G., Green, D., Hadasch, D., Hahn, A., Heckmann, L., Herrera, J., Hoang, J., Hrupec, D., HÃŒtten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jiménez, I., Jormanainen, J., Jouvin, L., Kajiwara, Y., Karjalainen, M., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López-Coto, R., López-Moya, M., López-Oramas, A., Loporchio, S., Machado De Oliveira Fraga, B., Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Menchiari, S., Mender, S., Mićanović, S., Miceli, D., Miener, T., Minev, M., Miranda, J. 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Abstract

In 2017, the Event Horizon Telescope (EHT) Collaboration succeeded in capturing the first direct image of the center of the M87 galaxy. The asymmetric ring morphology and size are consistent with theoretical expectations for a weakly accreting supermassive black hole of mass ∌6.5 × 109 M oË™. The EHTC also partnered with several international facilities in space and on the ground, to arrange an extensive, quasi-simultaneous multi-wavelength campaign. This Letter presents the results and analysis of this campaign, as well as the multi-wavelength data as a legacy data repository. We captured M87 in a historically low state, and the core flux dominates over HST-1 at high energies, making it possible to combine core flux constraints with the more spatially precise very long baseline interferometry data. We present the most complete simultaneous multi-wavelength spectrum of the active nucleus to date, and discuss the complexity and caveats of combining data from different spatial scales into one broadband spectrum. We apply two heuristic, isotropic leptonic single-zone models to provide insight into the basic source properties, but conclude that a structured jet is necessary to explain M87’s spectrum. We can exclude that the simultaneous γ-ray emission is produced via inverse Compton emission in the same region producing the EHT mm-band emission, and further conclude that the γ-rays can only be produced in the inner jets (inward of HST-1) if there are strongly particle-dominated regions. Direct synchrotron emission from accelerated protons and secondaries cannot yet be excluded. © 2021. The Author(s). Published by the American Astronomical Society..

Published
2021
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30. Broadband Multi-wavelength Properties of M87 during the 2017 Event Horizon Telescope Campaign

Author

Algaba, J. C., Anczarski, J., Asada, K., Baloković, M., Chandra, S., Cui, Y. -Z, Falcone, A. D., Giroletti, M., Goddi, C., Hada, K., Haggard, D., Jorstad, S., Kaur, A., Kawashima, T., Keating, G., Kim, J. -Y, Kino, M., Komossa, S., Kravchenko, E. V., Krichbaum, T. P., Lee, S. -S, Lu, R. -S, Lucchini, M., Markoff, S., Neilsen, J., Nowak, M. A., Park, J., Principe, G., Ramakrishnan, V., Reynolds, M. T., Sasada, M., Savchenko, S. S., Williamson, K. E., Akiyama, K., Alberdi, A., Alef, W., Anantua, R., Azulay, R., Baczko, A. -K, Ball, D., Barrett, J., Bintley, D., Benson, B. A., Blackburn, L., Blundell, R., Boland, W., Bouman, K. L., Bower, G. C., Boyce, H., Bremer, M., Brinkerink, C. D., Brissenden, R., Britzen, S., Broderick, A. E., Broguiere, D., Bronzwaer, T., Byun, D. -Y, Carlstrom, J. E., Chael, A., Chan, C. -K, Chatterjee, S., Chatterjee, K., Chen, M. -T, Chen, Y., Chesler, P. M., Cho, I., Christian, P., Conway, J. E., Cordes, J. M., Crawford, T. M., Crew, G. B., Cruz-Osorio, A., Davelaar, J., De Laurentis, M., Deane, R., Dempsey, J., Desvignes, G., Dexter, J., Doeleman, S. S., Eatough, R. P., Falcke, H., Farah, J., Fish, V. L., Fomalont, E., Ford, H. A., Fraga-Encinas, R., Friberg, P., Fromm, C. M., Fuentes, A., Galison, P., Gammie, C. F., García, R., Gentaz, O., Georgiev, B., Gold, R., Gómez, J. L., Gómez-Ruiz, A. I., Gu, M., Gurwell, M., Hecht, M. H., Hesper, R., Ho, L. C., Ho, P., Honma, M., Huang, C. -WL., Huang, L., Hughes, D. H., Ikeda, S., Inoue, M., Issaoun, S., James, D. J., Jannuzi, B. T., Janssen, M., Jeter, B., Jiang, W., Jiménez-Rosales, A., Johnson, M. D., Jung, T., Karami, M., Karuppusamy, R., Kettenis, M., Kim, D. -J, Kim, J., Koay, J. Y., Kofuji, Y., Koch, P. M., Koyama, S., Kramer, M., Kramer, C., Kuo, C. -Y, Lauer, T. R., Levis, A., Li, Y. -R, Li, Z., Lindqvist, M., Lico, R., Lindahl, G., Liu, J., Liu, K., Liuzzo, E., Lo, W. -P, Lobanov, A. P., Loinard, L., Lonsdale, C., Macdonald, N. 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Abstract

In 2017, the Event Horizon Telescope (EHT) Collaboration succeeded in capturing the first direct image of the center of the M87 galaxy. The asymmetric ring morphology and size are consistent with theoretical expectations for a weakly accreting supermassive black hole of mass ∌6.5 × 109 M oË™. The EHTC also partnered with several international facilities in space and on the ground, to arrange an extensive, quasi-simultaneous multi-wavelength campaign. This Letter presents the results and analysis of this campaign, as well as the multi-wavelength data as a legacy data repository. We captured M87 in a historically low state, and the core flux dominates over HST-1 at high energies, making it possible to combine core flux constraints with the more spatially precise very long baseline interferometry data. We present the most complete simultaneous multi-wavelength spectrum of the active nucleus to date, and discuss the complexity and caveats of combining data from different spatial scales into one broadband spectrum. We apply two heuristic, isotropic leptonic single-zone models to provide insight into the basic source properties, but conclude that a structured jet is necessary to explain M87’s spectrum. We can exclude that the simultaneous γ-ray emission is produced via inverse Compton emission in the same region producing the EHT mm-band emission, and further conclude that the γ-rays can only be produced in the inner jets (inward of HST-1) if there are strongly particle-dominated regions. Direct synchrotron emission from accelerated protons and secondaries cannot yet be excluded. © 2021. The Author(s). Published by the American Astronomical Society..

Published
2021
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31. Broadband Multi-wavelength Properties of M87 during the 2017 Event Horizon Telescope Campaign

Author

Algaba, J. C., Anczarski, J., Asada, K., Baloković, M., Chandra, S., Cui, Y. -Z, Falcone, A. D., Giroletti, M., Goddi, C., Hada, K., Haggard, D., Jorstad, S., Kaur, A., Kawashima, T., Keating, G., Kim, J. -Y, Kino, M., Komossa, S., Kravchenko, E. V., Krichbaum, T. P., Lee, S. -S, Lu, R. -S, Lucchini, M., Markoff, S., Neilsen, J., Nowak, M. A., Park, J., Principe, G., Ramakrishnan, V., Reynolds, M. T., Sasada, M., Savchenko, S. S., Williamson, K. E., Akiyama, K., Alberdi, A., Alef, W., Anantua, R., Azulay, R., Baczko, A. -K, Ball, D., Barrett, J., Bintley, D., Benson, B. A., Blackburn, L., Blundell, R., Boland, W., Bouman, K. L., Bower, G. C., Boyce, H., Bremer, M., Brinkerink, C. D., Brissenden, R., Britzen, S., Broderick, A. E., Broguiere, D., Bronzwaer, T., Byun, D. -Y, Carlstrom, J. E., Chael, A., Chan, C. -K, Chatterjee, S., Chatterjee, K., Chen, M. -T, Chen, Y., Chesler, P. M., Cho, I., Christian, P., Conway, J. E., Cordes, J. M., Crawford, T. M., Crew, G. 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Abstract

In 2017, the Event Horizon Telescope (EHT) Collaboration succeeded in capturing the first direct image of the center of the M87 galaxy. The asymmetric ring morphology and size are consistent with theoretical expectations for a weakly accreting supermassive black hole of mass ∌6.5 × 109 M oË™. The EHTC also partnered with several international facilities in space and on the ground, to arrange an extensive, quasi-simultaneous multi-wavelength campaign. This Letter presents the results and analysis of this campaign, as well as the multi-wavelength data as a legacy data repository. We captured M87 in a historically low state, and the core flux dominates over HST-1 at high energies, making it possible to combine core flux constraints with the more spatially precise very long baseline interferometry data. We present the most complete simultaneous multi-wavelength spectrum of the active nucleus to date, and discuss the complexity and caveats of combining data from different spatial scales into one broadband spectrum. We apply two heuristic, isotropic leptonic single-zone models to provide insight into the basic source properties, but conclude that a structured jet is necessary to explain M87’s spectrum. We can exclude that the simultaneous γ-ray emission is produced via inverse Compton emission in the same region producing the EHT mm-band emission, and further conclude that the γ-rays can only be produced in the inner jets (inward of HST-1) if there are strongly particle-dominated regions. Direct synchrotron emission from accelerated protons and secondaries cannot yet be excluded. © 2021. The Author(s). Published by the American Astronomical Society..

Published
2021
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32. Broadband Multi-wavelength Properties of M87 during the 2017 Event Horizon Telescope Campaign

Author

Algaba, J. C., Anczarski, J., Asada, K., Baloković, M., Chandra, S., Cui, Y. -Z, Falcone, A. D., Giroletti, M., Goddi, C., Hada, K., Haggard, D., Jorstad, S., Kaur, A., Kawashima, T., Keating, G., Kim, J. -Y, Kino, M., Komossa, S., Kravchenko, E. V., Krichbaum, T. P., Lee, S. -S, Lu, R. -S, Lucchini, M., Markoff, S., Neilsen, J., Nowak, M. A., Park, J., Principe, G., Ramakrishnan, V., Reynolds, M. T., Sasada, M., Savchenko, S. S., Williamson, K. E., Akiyama, K., Alberdi, A., Alef, W., Anantua, R., Azulay, R., Baczko, A. -K, Ball, D., Barrett, J., Bintley, D., Benson, B. A., Blackburn, L., Blundell, R., Boland, W., Bouman, K. L., Bower, G. C., Boyce, H., Bremer, M., Brinkerink, C. D., Brissenden, R., Britzen, S., Broderick, A. E., Broguiere, D., Bronzwaer, T., Byun, D. -Y, Carlstrom, J. E., Chael, A., Chan, C. -K, Chatterjee, S., Chatterjee, K., Chen, M. -T, Chen, Y., Chesler, P. M., Cho, I., Christian, P., Conway, J. E., Cordes, J. M., Crawford, T. M., Crew, G. B., Cruz-Osorio, A., Davelaar, J., De Laurentis, M., Deane, R., Dempsey, J., Desvignes, G., Dexter, J., Doeleman, S. S., Eatough, R. P., Falcke, H., Farah, J., Fish, V. L., Fomalont, E., Ford, H. A., Fraga-Encinas, R., Friberg, P., Fromm, C. M., Fuentes, A., Galison, P., Gammie, C. F., García, R., Gentaz, O., Georgiev, B., Gold, R., Gómez, J. L., Gómez-Ruiz, A. I., Gu, M., Gurwell, M., Hecht, M. H., Hesper, R., Ho, L. C., Ho, P., Honma, M., Huang, C. -WL., Huang, L., Hughes, D. H., Ikeda, S., Inoue, M., Issaoun, S., James, D. J., Jannuzi, B. T., Janssen, M., Jeter, B., Jiang, W., Jiménez-Rosales, A., Johnson, M. D., Jung, T., Karami, M., Karuppusamy, R., Kettenis, M., Kim, D. -J, Kim, J., Koay, J. Y., Kofuji, Y., Koch, P. M., Koyama, S., Kramer, M., Kramer, C., Kuo, C. -Y, Lauer, T. R., Levis, A., Li, Y. -R, Li, Z., Lindqvist, M., Lico, R., Lindahl, G., Liu, J., Liu, K., Liuzzo, E., Lo, W. -P, Lobanov, A. P., Loinard, L., Lonsdale, C., Macdonald, N. R., Mao, J., Marchili, N., Marrone, D. P., Marscher, A. P., Martí-Vidal, I., Matsushita, S., Matthews, L. D., Medeiros, L., Menten, K. M., Mizuno, I., Mizuno, Y., Moran, J. M., Moriyama, K., Moscibrodzka, M., MÃŒller, C., Musoke, G., Mejías, A. M., Nagai, H., Nagar, N. M., Nakamura, M., Narayan, R., Narayanan, G., Natarajan, I., Nathanail, A., Neri, R., Ni, C., Noutsos, A., Okino, H., Olivares, H., Ortiz-León, G. N., Oyama, T., Ozel, F., Palumbo, D. C. M., Patel, N., Pen, U. -L, Pesce, D. W., Piétu, V., Plambeck, R., Popstefanija, A., Porth, O., Pötzl, F. M., Prather, B., Preciado-López, J. A., Psaltis, D., Pu, H. -Y, Rao, R., Rawlings, M. G., Raymond, A. W., Rezzolla, L., Ricarte, A., Ripperda, B., Roelofs, F., Rogers, A., Ros, E., Rose, M., Roshanineshat, A., Rottmann, H., Roy, A. L., Ruszczyk, C., Rygl, K. L. J., Sánchez, S., Sánchez-Arguelles, D., Savolainen, T., Schloerb, F. P., Schuster, K. -F, Shao, L., Shen, Z., Small, D., Sohn, B. 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A., Prokoph, H., PÃŒhlhofer, G., Punch, Michael, Quirrenbach, A., Rauth, R., Reichherzer, P., Reimer, A., Reimer, O., Remy, Q., Renaud, M., Rieger, F., Rinchiuso, L., Romoli, C., Rowell, G., Rudak, B., Ruiz-Velasco, E., Sahakian, V., Sailer, S., Sanchez, D. A., Santangelo, A., Sasaki, M., Scalici, M., Schutte, H. M., Schwanke, U., Schwemmer, S., Seglar-Arroyo, M., Senniappan, M., Seyffert, A. S., Shafi, N., Shiningayamwe, K., Simoni, R., Sinha, A., Sol, H., Specovius, A., Spencer, S., Spir-Jacob, M., Stawarz, Ł., Sun, L., Steenkamp, R., Stegmann, C., Steinmassl, S., Steppa, C., Takahashi, T., Tavernier, T., Taylor, A. M., Terrier, R., Tiziani, D., Tluczykont, M., Tomankova, L., Trichard, C., Tsirou, M., Tuffs, R., Uchiyama, Y., Van Der Walt, D. J., Van Eldik, C., Van Rensburg, C., Van Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Vincent, P., Vink, J., Völk, H. J., Vuillaume, T., Wadiasingh, Z., Wagner, S. J., Watson, J., Werner, F., White, R., Wierzcholska, A., Wong, Y. W., Yusafzai, A., Zacharias, M., Zanin, R., Zargaryan, D., Zdziarski, A. A., Zech, A., Zhu, S. J., Zorn, J., Zouari, S., Å»ywucka, N., Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. A., Artero, M., Asano, K., Baack, D., Babić, A., Baquero, A., De Almeida, U. B., Barrio, J. A., Becerra González, J., Bednarek, W., Bellizzi, L., Bernardini, E., Bernardos, M., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., BoÅ¡njak, Åœ., Busetto, G., Carosi, R., Ceribella, G., Cerruti, M., Chai, Y., Chilingarian, A., Cikota, S., Colak, S. M., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D’Amico, G., D’Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Delgado Mendez, C., Depaoli, D., Di Pierro, F., Di Venere, L., Do Souto Espineira, E., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Ferrara, G., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., García López, R. J., Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Gliwny, P., Godinović, N., Green, J. G., Green, D., Hadasch, D., Hahn, A., Heckmann, L., Herrera, J., Hoang, J., Hrupec, D., HÃŒtten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jiménez, I., Jormanainen, J., Jouvin, L., Kajiwara, Y., Karjalainen, M., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López-Coto, R., López-Moya, M., López-Oramas, A., Loporchio, S., Machado De Oliveira Fraga, B., Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Menchiari, S., Mender, S., Mićanović, S., Miceli, D., Miener, T., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Neustroev, V., Nigro, C., Nilsson, K., Nishijima, K., Noda, K., Nozaki, S., Ohtani, Y., Oka, T., Otero-Santos, J., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pavletić, L., Penil, P., Perennes, C., Persic, M., Moroni, P. G. P., Prandini, E., Priyadarshi, C., Puljak, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Saturni, F. G., Schleicher, B., Schmidt, K., Schweizer, T., Sitarek, J., Å nidarić, I., Sobczynska, D., Spolon, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Surić, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Tosti, L., Truzzi, S., Tutone, A., Ubach, S., Van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Ventura, S., Verguilov, V., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Wunderlich, C., Zarić, D., Adams, C. B., Benbow, W., Brill, A., Capasso, M., Christiansen, J. L., Chromey, A. J., Daniel, M. K., Errando, M., Farrell, K. A., Feng, Q., Finley, J. P., Fortson, L., Furniss, A., Gent, A., Giuri, C., Hassan, T., Hervet, O., Holder, J., Hughes, G., Humensky, T. B., Jin, W., Kaaret, P., Kertzman, M., Kieda, D., Kumar, S., Lang, M. J., Lundy, M., Maier, G., Moriarty, P., Mukherjee, R., Nieto, D., Nievas-Rosillo, M., O’Brien, S., Ong, R. A., Otte, A. N., Patel, S., Pfrang, K., Pohl, M., Prado, R. R., Pueschel, E., Quinn, J., Ragan, K., Reynolds, P. T., Ribeiro, D., Richards, G. T., Roache, E., Rulten, C., Ryan, J. L., Santander, M., Sembroski, G. H., Shang, R., Weinstein, A., Williams, D. A., Williamson, T. J., Hirota, T., Cui, L., Niinuma, K., Ro, H., Sakai, N., Sawada-Satoh, S., Wajima, K., Wang, N., Liu, X., and Yonekura, Y.

Abstract

In 2017, the Event Horizon Telescope (EHT) Collaboration succeeded in capturing the first direct image of the center of the M87 galaxy. The asymmetric ring morphology and size are consistent with theoretical expectations for a weakly accreting supermassive black hole of mass ∌6.5 × 109 M oË™. The EHTC also partnered with several international facilities in space and on the ground, to arrange an extensive, quasi-simultaneous multi-wavelength campaign. This Letter presents the results and analysis of this campaign, as well as the multi-wavelength data as a legacy data repository. We captured M87 in a historically low state, and the core flux dominates over HST-1 at high energies, making it possible to combine core flux constraints with the more spatially precise very long baseline interferometry data. We present the most complete simultaneous multi-wavelength spectrum of the active nucleus to date, and discuss the complexity and caveats of combining data from different spatial scales into one broadband spectrum. We apply two heuristic, isotropic leptonic single-zone models to provide insight into the basic source properties, but conclude that a structured jet is necessary to explain M87’s spectrum. We can exclude that the simultaneous γ-ray emission is produced via inverse Compton emission in the same region producing the EHT mm-band emission, and further conclude that the γ-rays can only be produced in the inner jets (inward of HST-1) if there are strongly particle-dominated regions. Direct synchrotron emission from accelerated protons and secondaries cannot yet be excluded. © 2021. The Author(s). Published by the American Astronomical Society..

Published
2021
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33. Organic chemistry in the protosolar analogue HOPS-108: Environment matters

Author

Chahine, L., López-Sepulcre, A., Neri, R., Ceccarelli, C., Mercimek, S., Codella, C., Bouvier, M., Bianchi, E., Favre, C., Podio, L., Alves, F. O., Sakai, N., Yamamoto, S., Chahine, L., López-Sepulcre, A., Neri, R., Ceccarelli, C., Mercimek, S., Codella, C., Bouvier, M., Bianchi, E., Favre, C., Podio, L., Alves, F. O., Sakai, N., and Yamamoto, S.

Abstract

Hot corinos are compact regions around solar-mass protostellar objects that are very rich in interstellar complex organic molecules (iCOMs). They are believed to represent the very early phases of our Solar System's birth, which was very likely also characterized by rich organic chemistry. While most of the studied hot corinos are either isolated or born in a loose protocluster, our Sun was born in a densely packed star cluster, near massive stars whose ultraviolet radiation must have contributed to shaping the evolution of the surrounding environment. In addition, internal irradiation from energetic particles ($>$10 Mev), whose imprint is seen today in the products of short-lived radionuclides in meteoritic material, is also known to have occurred during the Solar System formation. How did all these conditions affect the chemistry of the proto-Sun and its surroundings is still an open question. To answer this question, we studied HOPS-108, the hot corino located in the protosolar analogue OMC-2 FIR4. The study was carried out with ALMA at 1.3mm with an angular resolution of $\sim$100 AU. We detected 11 iCOMs such as CH$_{3}$OH HCOOCH$_{3}$ and CH$_{3}$OCH$_{3}$. Our results can be summarized as follows: (1) an enhancement of HCOOCH3 with respect to other hot corinos, (2) a [CH$_{3}$OCH$_{3}$]/[HCOOCH$_{3}$] abundance ratio of $\sim$0.2 marginally deviating from the usual trend seen in other sources ([CH$_{3}$OCH$_{3}$]/[HCOOCH$_{3}$] $\sim$1), (3) a [CH$_{2}$DOH]/[CH$_{3}$OH] ratio of 2.5\% which is lower than what is seen in Perseus and Ophiuchus hot corinos ($\sim$7\%-9\%) and similar to that seen in HH212 another source located in Orion. This might result from different physical conditions in the Orion molecular complex compared to other regions.

Published
2021
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34. The SVS13-A Class I chemical complexity as revealed by S-bearing species. SOLIS XIII

Author

Codella, C., Bianchi, E., Podio, L., Mercimek, S., Ceccarelli, C., Lopez-Sepulcre, A., Bachiller, R., Caselli, P., Sakai, N., Neri, R., Fontani, F., Favre, C., Balucani, N., Lefloch, B., Viti, S., Yamamoto, S., Codella, C., Bianchi, E., Podio, L., Mercimek, S., Ceccarelli, C., Lopez-Sepulcre, A., Bachiller, R., Caselli, P., Sakai, N., Neri, R., Fontani, F., Favre, C., Balucani, N., Lefloch, B., Viti, S., and Yamamoto, S.

Abstract

Aims: The goal is to obtain a census of S-bearing species using interferometric images, towards SVS13-A, a Class I object associated with a hot corino rich in interstellar complex organic molecules. Methods: We used data at 3mm and 1.4mm obtained with IRAM-NOEMA in the framework of the Large Program SOLIS. Results: We imaged the spatial distribution of the line emission of 32SO, 34SO, C32}S, C34S, C33S, OCS, H2C32S, H2C34S, and NS. The low excitation (9 K) 32SO line is tracing the fast collimated jet driven by the nearby SVS13-B. Conversely, the rest of the lines are confined in the inner SVS13-A region, where complex organics have been previously imaged. The non-LTE LVG analysis of SO, SO2, and H2CS indicates a hot corino origin (60-120 au). Temperatures between 50 K and 300 K, and volume densities larger than 10^5 cm-3 have been derived. The abundances are in the following ranges: 0.3-6 10^-6 (CS), 7 10^-9} - 1 10^-7 (SO), 1-10 10^-7 (SO2), a few 10^-10 (H2CS and OCS), and 10^{-10} - 10^{-9}(NS). The N(NS)/N(NS^+) ratio is larger than 10, supporting that the NS^+ ion is mainly formed in the extended envelope. Conclusions: The [H2CS]/[H2CO] ratio increases with time (from Class 0 to Class II objects) by more than one order of magnitude. This suggests that [S]/[O] changes along the Sun-like star forming process. The estimate of the [S]/[H] budget in SVS13-A is 2%-17% of the Solar System value (1.8 10^-5), being consistent with what was previously measured towards Class 0 objects (1%-8%). This supports that the enrichment of the sulphuretted species with respect to dark clouds keeps constant from the Class 0 to the Class I stages of low-mass star formation. The present findings stress the importance of investigating the chemistry of star forming regions using large observational surveys as well as sampling regions on a Solar System scale., Comment: A&A, in press

Published
2021
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35. ORion Alma New GEneration Survey (ORANGES) I. Dust continuum and free-free emission of OMC-2/3 filament protostars

Author

Bouvier, M., López-Sepulcre, A., Ceccarelli, C., Sakai, N., Yamamoto, S., Yang, Y-L., Bouvier, M., López-Sepulcre, A., Ceccarelli, C., Sakai, N., Yamamoto, S., and Yang, Y-L.

Abstract

The spectral energy distribution (SED) in the millimetre (mm) to centimetre (cm) range is a useful tool for characterising the dust in protostellar envelopes as well as free-free emission from the protostar and outflow. While many studies have been carried out towards low- and high-mass protostars, little exists so far about solar-type protostars in high-mass star-forming regions, which are likely to be representatives of the conditions where the Solar System was born. We focus here on the OMC-2/3 solar-type protostars, which are bounded by nearby HII regions and which are, therefore, potentially affected by the high-UV illumination. We aim to understand whether the small-scale structure ($\leq$1000 au) and the evolutionary status of these solar-type protostars are affected by the nearby HII regions, as is the case for the large-scale ($\leq$10$^4$ au) gas chemical composition. We used ALMA in the 1.3 mm band (246.2 GHz) to image the continuum of 16 OMC-2/3 solar-type protostars, with an angular resolution of 0.25$''$ (100 au). We completed our data with archival data from the VANDAM survey of Orion Protostars at 333 and 32.9 GHz, respectively, to construct the dust SED, extract several dust parameters and to assess whether free-free emission is contaminating their dust SED in the cm range. From the mm to cm range dust SED, we found low dust emissivity spectral indexes ($\beta < 1$) for the majority of our source sample and free-free emission towards only 5 of the 16 sample sources. We were also able to confirm or correct the evolutionary status of the source sample. Finally, we did not find any dependence of the source dust parameters on their location in the OMC-2/3 filament. Our results show that the small-scale dust properties of the OMC-2/3 protostars are not affected by the high- UV illumination from the nearby HII regions., Comment: 30 pages, 14 figures, Accepted for publication in A&A

Published
2021
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36. Global impact of COVID-19 on stroke care

Author

Nogueira, RG, Abdalkader, M, Qureshi, MM, Frankel, MR, Mansour, OY, Yamagami, H, Qiu, Z, Farhoudi, M, Siegler, JE, Yaghi, S, Raz, E, Sakai, N, Ohara, N, Piotin, M, Mechtouff, L, Eker, O, Chalumeau, V, Kleinig, TJ, Pop, R, Liu, J, Winters, HS, Shang, X, Rodriguez Vasquez, A, Blasco, J, Arenillas, JF, Martinez-Galdamez, M, Brehm, A, Psychogios, M-N, Lylyk, P, Haussen, DC, Al-Bayati, AR, Mohammaden, MH, Fonseca, L, Luis Silva, M, Montalverne, F, Renieri, L, Mangiafico, S, Fischer, U, Gralla, J, Frei, D, Chugh, C, Mehta, BP, Nagel, S, Mohlenbruch, M, Ortega-Gutierrez, S, Farooqui, M, Hassan, AE, Taylor, A, Lapergue, B, Consoli, A, Campbell, BCV, Sharma, M, Walker, M, Van Horn, N, Fiehler, J, Huy, TN, Nguyen, QT, Watanabe, D, Zhang, H, Le, HV, Nguyen, VQ, Shah, R, Devlin, T, Khandelwal, P, Linfante, I, Izzath, W, Lavados, PM, Olavarria, VV, Silva, GS, de Carvalho Sousa, AV, Kirmani, J, Bendszus, M, Amano, T, Yamamoto, R, Doijiri, R, Tokuda, N, Yamada, T, Terasaki, T, Yazawa, Y, Morris, JG, Griffin, E, Thornton, J, Lavoie, P, Matouk, C, Hill, MD, Demchuk, AM, Killer-Oberpfalzer, M, Nahab, F, Altschul, D, Ramos-Pachon, A, Perez de la Ossa, N, Kikano, R, Boisseau, W, Walker, G, Cordina, SM, Puri, A, Kuhn, AL, Gandhi, D, Ramakrishnan, P, Novakovic-White, R, Chebl, A, Kargiotis, O, Czap, A, Zha, A, Masoud, HE, Lopez, C, Ozretic, D, Al-Mufti, F, Zie, W, Duan, Z, Yuan, Z, Huang, W, Hao, Y, Luo, J, Kalousek, V, Bourcier, R, Guile, R, Hetts, S, Al-Jehani, HM, AlHazzani, A, Sadeghi-Hokmabadi, E, Teleb, M, Payne, J, Lee, JS, Hong, JM, Sohn, S-I, Hwang, Y-H, Shin, DH, Roh, HG, Edgell, R, Khatri, R, Smith, A, Malik, A, Liebeskind, D, Herial, N, Jabbour, P, Magalhaes, P, Ozdemir, AO, Aykac, O, Uwatoko, T, Dembo, T, Shimizu, H, Sugiura, Y, Miyashita, F, Fukuda, H, Miyake, K, Shimbo, J, Sugimura, Y, Beer-Furlan, A, Joshi, K, Catanese, L, Abud, DG, Pontes Neto, O, Mehrpour, M, Al Hashmi, A, Saqqur, M, Mostafa, A, Fifi, JT, Hussain, S, John, S, Gupta, R, Sivan-Hoffmann, R, Reznik, A, Sani, AF, Geyik, S, Akil, ECR, Churojana, A, Ghoreishi, A, Saadatnia, M, Sharifipour, E, Ma, A, Faulder, K, Wu, T, Leung, L, Malek, A, Voetsch, B, Wakhloo, A, Rivera, R, Barrientos Iman, DM, Pikula, A, Lioutas, V-A, Thomalla, G, Birnbaum, L, Machi, P, Bernava, G, McDermott, M, Kleindorfer, D, Wong, K, Patterson, MS, Fiorot, JA, Huded, V, Mack, W, Tenser, M, Eskey, C, Multani, S, Kelly, M, Janardhan, V, Cornett, O, Singh, V, Murayama, Y, Mokin, M, Yang, P, Zhang, X, Yin, C, Han, H, Peng, Y, Chen, W, Crosa, R, Frudit, ME, Pandian, JD, Kulkarni, A, Yagita, Y, Takenobu, Y, Matsumaru, Y, Yamada, S, Kono, R, Kanamaru, T, Yamazaki, H, Sakaguchi, M, Todo, K, Yamamoto, N, Sonoda, K, Yoshida, T, Hashimoto, H, Nakahara, I, Cora, E, Volders, D, Ducroux, C, Shoamanesh, A, Ospel, J, Kaliaev, A, Ahmed, S, Rashid, U, Rebello, LC, Pereira, VM, Fahed, R, Chen, M, Sheth, SA, Palaiodimou, L, Tsivgoulis, G, Chandra, R, Koyfman, F, Leung, T, Khosravani, H, Dharmadhikari, S, Frisullo, G, Calabresi, P, Tsiskaridze, A, Lobjanidze, N, Grigoryan, M, Czlonkowska, A, de Sousa, DA, Demeestere, J, Liang, C, Sangha, N, Lutsep, HL, Ayo-Martin, O, Cruz-Culebras, A, Tran, AD, Young, CY, Cordonnier, C, Caparros, F, Alonso De Lecinana, M, Fuentes, B, Yavagal, D, Jovin, T, Spelle, L, Moret, J, Khatri, P, Zaidat, O, Raymond, J, Martins, S, Thanh, N, Nogueira, RG, Abdalkader, M, Qureshi, MM, Frankel, MR, Mansour, OY, Yamagami, H, Qiu, Z, Farhoudi, M, Siegler, JE, Yaghi, S, Raz, E, Sakai, N, Ohara, N, Piotin, M, Mechtouff, L, Eker, O, Chalumeau, V, Kleinig, TJ, Pop, R, Liu, J, Winters, HS, Shang, X, Rodriguez Vasquez, A, Blasco, J, Arenillas, JF, Martinez-Galdamez, M, Brehm, A, Psychogios, M-N, Lylyk, P, Haussen, DC, Al-Bayati, AR, Mohammaden, MH, Fonseca, L, Luis Silva, M, Montalverne, F, Renieri, L, Mangiafico, S, Fischer, U, Gralla, J, Frei, D, Chugh, C, Mehta, BP, Nagel, S, Mohlenbruch, M, Ortega-Gutierrez, S, Farooqui, M, Hassan, AE, Taylor, A, Lapergue, B, Consoli, A, Campbell, BCV, Sharma, M, Walker, M, Van Horn, N, Fiehler, J, Huy, TN, Nguyen, QT, Watanabe, D, Zhang, H, Le, HV, Nguyen, VQ, Shah, R, Devlin, T, Khandelwal, P, Linfante, I, Izzath, W, Lavados, PM, Olavarria, VV, Silva, GS, de Carvalho Sousa, AV, Kirmani, J, Bendszus, M, Amano, T, Yamamoto, R, Doijiri, R, Tokuda, N, Yamada, T, Terasaki, T, Yazawa, Y, Morris, JG, Griffin, E, Thornton, J, Lavoie, P, Matouk, C, Hill, MD, Demchuk, AM, Killer-Oberpfalzer, M, Nahab, F, Altschul, D, Ramos-Pachon, A, Perez de la Ossa, N, Kikano, R, Boisseau, W, Walker, G, Cordina, SM, Puri, A, Kuhn, AL, Gandhi, D, Ramakrishnan, P, Novakovic-White, R, Chebl, A, Kargiotis, O, Czap, A, Zha, A, Masoud, HE, Lopez, C, Ozretic, D, Al-Mufti, F, Zie, W, Duan, Z, Yuan, Z, Huang, W, Hao, Y, Luo, J, Kalousek, V, Bourcier, R, Guile, R, Hetts, S, Al-Jehani, HM, AlHazzani, A, Sadeghi-Hokmabadi, E, Teleb, M, Payne, J, Lee, JS, Hong, JM, Sohn, S-I, Hwang, Y-H, Shin, DH, Roh, HG, Edgell, R, Khatri, R, Smith, A, Malik, A, Liebeskind, D, Herial, N, Jabbour, P, Magalhaes, P, Ozdemir, AO, Aykac, O, Uwatoko, T, Dembo, T, Shimizu, H, Sugiura, Y, Miyashita, F, Fukuda, H, Miyake, K, Shimbo, J, Sugimura, Y, Beer-Furlan, A, Joshi, K, Catanese, L, Abud, DG, Pontes Neto, O, Mehrpour, M, Al Hashmi, A, Saqqur, M, Mostafa, A, Fifi, JT, Hussain, S, John, S, Gupta, R, Sivan-Hoffmann, R, Reznik, A, Sani, AF, Geyik, S, Akil, ECR, Churojana, A, Ghoreishi, A, Saadatnia, M, Sharifipour, E, Ma, A, Faulder, K, Wu, T, Leung, L, Malek, A, Voetsch, B, Wakhloo, A, Rivera, R, Barrientos Iman, DM, Pikula, A, Lioutas, V-A, Thomalla, G, Birnbaum, L, Machi, P, Bernava, G, McDermott, M, Kleindorfer, D, Wong, K, Patterson, MS, Fiorot, JA, Huded, V, Mack, W, Tenser, M, Eskey, C, Multani, S, Kelly, M, Janardhan, V, Cornett, O, Singh, V, Murayama, Y, Mokin, M, Yang, P, Zhang, X, Yin, C, Han, H, Peng, Y, Chen, W, Crosa, R, Frudit, ME, Pandian, JD, Kulkarni, A, Yagita, Y, Takenobu, Y, Matsumaru, Y, Yamada, S, Kono, R, Kanamaru, T, Yamazaki, H, Sakaguchi, M, Todo, K, Yamamoto, N, Sonoda, K, Yoshida, T, Hashimoto, H, Nakahara, I, Cora, E, Volders, D, Ducroux, C, Shoamanesh, A, Ospel, J, Kaliaev, A, Ahmed, S, Rashid, U, Rebello, LC, Pereira, VM, Fahed, R, Chen, M, Sheth, SA, Palaiodimou, L, Tsivgoulis, G, Chandra, R, Koyfman, F, Leung, T, Khosravani, H, Dharmadhikari, S, Frisullo, G, Calabresi, P, Tsiskaridze, A, Lobjanidze, N, Grigoryan, M, Czlonkowska, A, de Sousa, DA, Demeestere, J, Liang, C, Sangha, N, Lutsep, HL, Ayo-Martin, O, Cruz-Culebras, A, Tran, AD, Young, CY, Cordonnier, C, Caparros, F, Alonso De Lecinana, M, Fuentes, B, Yavagal, D, Jovin, T, Spelle, L, Moret, J, Khatri, P, Zaidat, O, Raymond, J, Martins, S, and Thanh, N

Abstract

BACKGROUND: The COVID-19 pandemic led to profound changes in the organization of health care systems worldwide. AIMS: We sought to measure the global impact of the COVID-19 pandemic on the volumes for mechanical thrombectomy, stroke, and intracranial hemorrhage hospitalizations over a three-month period at the height of the pandemic (1 March-31 May 2020) compared with two control three-month periods (immediately preceding and one year prior). METHODS: Retrospective, observational, international study, across 6 continents, 40 countries, and 187 comprehensive stroke centers. The diagnoses were identified by their ICD-10 codes and/or classifications in stroke databases at participating centers. RESULTS: The hospitalization volumes for any stroke, intracranial hemorrhage, and mechanical thrombectomy were 26,699, 4002, and 5191 in the three months immediately before versus 21,576, 3540, and 4533 during the first three pandemic months, representing declines of 19.2% (95%CI, -19.7 to -18.7), 11.5% (95%CI, -12.6 to -10.6), and 12.7% (95%CI, -13.6 to -11.8), respectively. The decreases were noted across centers with high, mid, and low COVID-19 hospitalization burden, and also across high, mid, and low volume stroke/mechanical thrombectomy centers. High-volume COVID-19 centers (-20.5%) had greater declines in mechanical thrombectomy volumes than mid- (-10.1%) and low-volume (-8.7%) centers (p < 0.0001). There was a 1.5% stroke rate across 54,366 COVID-19 hospitalizations. SARS-CoV-2 infection was noted in 3.9% (784/20,250) of all stroke admissions. CONCLUSION: The COVID-19 pandemic was associated with a global decline in the volume of overall stroke hospitalizations, mechanical thrombectomy procedures, and intracranial hemorrhage admission volumes. Despite geographic variations, these volume reductions were observed regardless of COVID-19 hospitalization burden and pre-pandemic stroke/mechanical thrombectomy volumes.

Published
2021

37. Broadband Multi-wavelength Properties of M87 during the 2017 Event Horizon Telescope Campaign

Author

Algaba, J. C., Anczarski, J., Asada, K., Baloković, M., Chandra, S., Cui, Y. -Z, Falcone, A. D., Giroletti, M., Goddi, C., Hada, K., Haggard, D., Jorstad, S., Kaur, A., Kawashima, T., Keating, G., Kim, J. -Y, Kino, M., Komossa, S., Kravchenko, E. V., Krichbaum, T. P., Lee, S. -S, Lu, R. -S, Lucchini, M., Markoff, S., Neilsen, J., Nowak, M. A., Park, J., Principe, G., Ramakrishnan, V., Reynolds, M. T., Sasada, M., Savchenko, S. S., Williamson, K. E., Akiyama, K., Alberdi, A., Alef, W., Anantua, R., Azulay, R., Baczko, A. -K, Ball, D., Barrett, J., Bintley, D., Benson, B. A., Blackburn, L., Blundell, R., Boland, W., Bouman, K. L., Bower, G. C., Boyce, H., Bremer, M., Brinkerink, C. D., Brissenden, R., Britzen, S., Broderick, A. E., Broguiere, D., Bronzwaer, T., Byun, D. -Y, Carlstrom, J. E., Chael, A., Chan, C. -K, Chatterjee, S., Chatterjee, K., Chen, M. -T, Chen, Y., Chesler, P. M., Cho, I., Christian, P., Conway, J. E., Cordes, J. M., Crawford, T. M., Crew, G. B., Cruz-Osorio, A., Davelaar, J., De Laurentis, M., Deane, R., Dempsey, J., Desvignes, G., Dexter, J., Doeleman, S. S., Eatough, R. P., Falcke, H., Farah, J., Fish, V. L., Fomalont, E., Ford, H. A., Fraga-Encinas, R., Friberg, P., Fromm, C. M., Fuentes, A., Galison, P., Gammie, C. F., García, R., Gentaz, O., Georgiev, B., Gold, R., Gómez, J. L., Gómez-Ruiz, A. I., Gu, M., Gurwell, M., Hecht, M. H., Hesper, R., Ho, L. C., Ho, P., Honma, M., Huang, C. -WL., Huang, L., Hughes, D. H., Ikeda, S., Inoue, M., Issaoun, S., James, D. J., Jannuzi, B. T., Janssen, M., Jeter, B., Jiang, W., Jiménez-Rosales, A., Johnson, M. D., Jung, T., Karami, M., Karuppusamy, R., Kettenis, M., Kim, D. -J, Kim, J., Koay, J. Y., Kofuji, Y., Koch, P. M., Koyama, S., Kramer, M., Kramer, C., Kuo, C. -Y, Lauer, T. R., Levis, A., Li, Y. -R, Li, Z., Lindqvist, M., Lico, R., Lindahl, G., Liu, J., Liu, K., Liuzzo, E., Lo, W. -P, Lobanov, A. P., Loinard, L., Lonsdale, C., Macdonald, N. 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W., Yusafzai, A., Zacharias, M., Zanin, R., Zargaryan, D., Zdziarski, A. A., Zech, A., Zhu, S. J., Zorn, J., Zouari, S., Å»ywucka, N., Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. A., Artero, M., Asano, K., Baack, D., Babić, A., Baquero, A., De Almeida, U. B., Barrio, J. A., Becerra González, J., Bednarek, W., Bellizzi, L., Bernardini, E., Bernardos, M., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., BoÅ¡njak, Åœ., Busetto, G., Carosi, R., Ceribella, G., Cerruti, M., Chai, Y., Chilingarian, A., Cikota, S., Colak, S. M., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D’Amico, G., D’Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Delgado Mendez, C., Depaoli, D., Di Pierro, F., Di Venere, L., Do Souto Espineira, E., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Elsaesser, D., Fallah Ramazani, V., Fattorini, A., Ferrara, G., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., García López, R. J., Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Gliwny, P., Godinović, N., Green, J. G., Green, D., Hadasch, D., Hahn, A., Heckmann, L., Herrera, J., Hoang, J., Hrupec, D., HÃŒtten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jiménez, I., Jormanainen, J., Jouvin, L., Kajiwara, Y., Karjalainen, M., Kerszberg, D., Kobayashi, Y., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López-Coto, R., López-Moya, M., López-Oramas, A., Loporchio, S., Machado De Oliveira Fraga, B., Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Menchiari, S., Mender, S., Mićanović, S., Miceli, D., Miener, T., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Neustroev, V., Nigro, C., Nilsson, K., Nishijima, K., Noda, K., Nozaki, S., Ohtani, Y., Oka, T., Otero-Santos, J., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pavletić, L., Penil, P., Perennes, C., Persic, M., Moroni, P. G. P., Prandini, E., Priyadarshi, C., Puljak, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Saturni, F. G., Schleicher, B., Schmidt, K., Schweizer, T., Sitarek, J., Å nidarić, I., Sobczynska, D., Spolon, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Surić, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Tosti, L., Truzzi, S., Tutone, A., Ubach, S., Van Scherpenberg, J., Vanzo, G., Vazquez Acosta, M., Ventura, S., Verguilov, V., Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Wunderlich, C., Zarić, D., Adams, C. B., Benbow, W., Brill, A., Capasso, M., Christiansen, J. L., Chromey, A. J., Daniel, M. K., Errando, M., Farrell, K. A., Feng, Q., Finley, J. P., Fortson, L., Furniss, A., Gent, A., Giuri, C., Hassan, T., Hervet, O., Holder, J., Hughes, G., Humensky, T. B., Jin, W., Kaaret, P., Kertzman, M., Kieda, D., Kumar, S., Lang, M. J., Lundy, M., Maier, G., Moriarty, P., Mukherjee, R., Nieto, D., Nievas-Rosillo, M., O’Brien, S., Ong, R. A., Otte, A. N., Patel, S., Pfrang, K., Pohl, M., Prado, R. R., Pueschel, E., Quinn, J., Ragan, K., Reynolds, P. T., Ribeiro, D., Richards, G. T., Roache, E., Rulten, C., Ryan, J. L., Santander, M., Sembroski, G. H., Shang, R., Weinstein, A., Williams, D. A., Williamson, T. J., Hirota, T., Cui, L., Niinuma, K., Ro, H., Sakai, N., Sawada-Satoh, S., Wajima, K., Wang, N., Liu, X., and Yonekura, Y.

Abstract

In 2017, the Event Horizon Telescope (EHT) Collaboration succeeded in capturing the first direct image of the center of the M87 galaxy. The asymmetric ring morphology and size are consistent with theoretical expectations for a weakly accreting supermassive black hole of mass ∌6.5 × 109 M oË™. The EHTC also partnered with several international facilities in space and on the ground, to arrange an extensive, quasi-simultaneous multi-wavelength campaign. This Letter presents the results and analysis of this campaign, as well as the multi-wavelength data as a legacy data repository. We captured M87 in a historically low state, and the core flux dominates over HST-1 at high energies, making it possible to combine core flux constraints with the more spatially precise very long baseline interferometry data. We present the most complete simultaneous multi-wavelength spectrum of the active nucleus to date, and discuss the complexity and caveats of combining data from different spatial scales into one broadband spectrum. We apply two heuristic, isotropic leptonic single-zone models to provide insight into the basic source properties, but conclude that a structured jet is necessary to explain M87’s spectrum. We can exclude that the simultaneous γ-ray emission is produced via inverse Compton emission in the same region producing the EHT mm-band emission, and further conclude that the γ-rays can only be produced in the inner jets (inward of HST-1) if there are strongly particle-dominated regions. Direct synchrotron emission from accelerated protons and secondaries cannot yet be excluded. © 2021. The Author(s). Published by the American Astronomical Society..

Published
2021
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38. Organic chemistry in the protosolar analogue HOPS-108: Environment matters

Author

Chahine, L., López-Sepulcre, A., Neri, R., Ceccarelli, C., Mercimek, S., Codella, C., Bouvier, M., Bianchi, E., Favre, C., Podio, L., Alves, F. O., Sakai, N., Yamamoto, S., Chahine, L., López-Sepulcre, A., Neri, R., Ceccarelli, C., Mercimek, S., Codella, C., Bouvier, M., Bianchi, E., Favre, C., Podio, L., Alves, F. O., Sakai, N., and Yamamoto, S.

Abstract

Hot corinos are compact regions around solar-mass protostellar objects that are very rich in interstellar complex organic molecules (iCOMs). They are believed to represent the very early phases of our Solar System's birth, which was very likely also characterized by rich organic chemistry. While most of the studied hot corinos are either isolated or born in a loose protocluster, our Sun was born in a densely packed star cluster, near massive stars whose ultraviolet radiation must have contributed to shaping the evolution of the surrounding environment. In addition, internal irradiation from energetic particles ($>$10 Mev), whose imprint is seen today in the products of short-lived radionuclides in meteoritic material, is also known to have occurred during the Solar System formation. How did all these conditions affect the chemistry of the proto-Sun and its surroundings is still an open question. To answer this question, we studied HOPS-108, the hot corino located in the protosolar analogue OMC-2 FIR4. The study was carried out with ALMA at 1.3mm with an angular resolution of $\sim$100 AU. We detected 11 iCOMs such as CH$_{3}$OH HCOOCH$_{3}$ and CH$_{3}$OCH$_{3}$. Our results can be summarized as follows: (1) an enhancement of HCOOCH3 with respect to other hot corinos, (2) a [CH$_{3}$OCH$_{3}$]/[HCOOCH$_{3}$] abundance ratio of $\sim$0.2 marginally deviating from the usual trend seen in other sources ([CH$_{3}$OCH$_{3}$]/[HCOOCH$_{3}$] $\sim$1), (3) a [CH$_{2}$DOH]/[CH$_{3}$OH] ratio of 2.5\% which is lower than what is seen in Perseus and Ophiuchus hot corinos ($\sim$7\%-9\%) and similar to that seen in HH212 another source located in Orion. This might result from different physical conditions in the Orion molecular complex compared to other regions.

Published
2021
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39. The SVS13-A Class I chemical complexity as revealed by S-bearing species. SOLIS XIII

Author

Codella, C., Bianchi, E., Podio, L., Mercimek, S., Ceccarelli, C., Lopez-Sepulcre, A., Bachiller, R., Caselli, P., Sakai, N., Neri, R., Fontani, F., Favre, C., Balucani, N., Lefloch, B., Viti, S., Yamamoto, S., Codella, C., Bianchi, E., Podio, L., Mercimek, S., Ceccarelli, C., Lopez-Sepulcre, A., Bachiller, R., Caselli, P., Sakai, N., Neri, R., Fontani, F., Favre, C., Balucani, N., Lefloch, B., Viti, S., and Yamamoto, S.

Abstract

Aims: The goal is to obtain a census of S-bearing species using interferometric images, towards SVS13-A, a Class I object associated with a hot corino rich in interstellar complex organic molecules. Methods: We used data at 3mm and 1.4mm obtained with IRAM-NOEMA in the framework of the Large Program SOLIS. Results: We imaged the spatial distribution of the line emission of 32SO, 34SO, C32}S, C34S, C33S, OCS, H2C32S, H2C34S, and NS. The low excitation (9 K) 32SO line is tracing the fast collimated jet driven by the nearby SVS13-B. Conversely, the rest of the lines are confined in the inner SVS13-A region, where complex organics have been previously imaged. The non-LTE LVG analysis of SO, SO2, and H2CS indicates a hot corino origin (60-120 au). Temperatures between 50 K and 300 K, and volume densities larger than 10^5 cm-3 have been derived. The abundances are in the following ranges: 0.3-6 10^-6 (CS), 7 10^-9} - 1 10^-7 (SO), 1-10 10^-7 (SO2), a few 10^-10 (H2CS and OCS), and 10^{-10} - 10^{-9}(NS). The N(NS)/N(NS^+) ratio is larger than 10, supporting that the NS^+ ion is mainly formed in the extended envelope. Conclusions: The [H2CS]/[H2CO] ratio increases with time (from Class 0 to Class II objects) by more than one order of magnitude. This suggests that [S]/[O] changes along the Sun-like star forming process. The estimate of the [S]/[H] budget in SVS13-A is 2%-17% of the Solar System value (1.8 10^-5), being consistent with what was previously measured towards Class 0 objects (1%-8%). This supports that the enrichment of the sulphuretted species with respect to dark clouds keeps constant from the Class 0 to the Class I stages of low-mass star formation. The present findings stress the importance of investigating the chemistry of star forming regions using large observational surveys as well as sampling regions on a Solar System scale., Comment: A&A, in press

Published
2021
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40. ORion Alma New GEneration Survey (ORANGES) I. Dust continuum and free-free emission of OMC-2/3 filament protostars

Author

Bouvier, M., López-Sepulcre, A., Ceccarelli, C., Sakai, N., Yamamoto, S., Yang, Y-L., Bouvier, M., López-Sepulcre, A., Ceccarelli, C., Sakai, N., Yamamoto, S., and Yang, Y-L.

Abstract

The spectral energy distribution (SED) in the millimetre (mm) to centimetre (cm) range is a useful tool for characterising the dust in protostellar envelopes as well as free-free emission from the protostar and outflow. While many studies have been carried out towards low- and high-mass protostars, little exists so far about solar-type protostars in high-mass star-forming regions, which are likely to be representatives of the conditions where the Solar System was born. We focus here on the OMC-2/3 solar-type protostars, which are bounded by nearby HII regions and which are, therefore, potentially affected by the high-UV illumination. We aim to understand whether the small-scale structure ($\leq$1000 au) and the evolutionary status of these solar-type protostars are affected by the nearby HII regions, as is the case for the large-scale ($\leq$10$^4$ au) gas chemical composition. We used ALMA in the 1.3 mm band (246.2 GHz) to image the continuum of 16 OMC-2/3 solar-type protostars, with an angular resolution of 0.25$''$ (100 au). We completed our data with archival data from the VANDAM survey of Orion Protostars at 333 and 32.9 GHz, respectively, to construct the dust SED, extract several dust parameters and to assess whether free-free emission is contaminating their dust SED in the cm range. From the mm to cm range dust SED, we found low dust emissivity spectral indexes ($\beta < 1$) for the majority of our source sample and free-free emission towards only 5 of the 16 sample sources. We were also able to confirm or correct the evolutionary status of the source sample. Finally, we did not find any dependence of the source dust parameters on their location in the OMC-2/3 filament. Our results show that the small-scale dust properties of the OMC-2/3 protostars are not affected by the high- UV illumination from the nearby HII regions., Comment: 30 pages, 14 figures, Accepted for publication in A&A

Published
2021
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41. FAUST I. The hot corino at the heart of the prototypical Class I protostar L1551 IRS5

Author

Bianchi, E., Chandler, C. J., Ceccarelli, C., Codella, C., Sakai, N., López-Sepulcre, A., Maud, L. T., Moellenbrock, G., Svoboda, B., Watanabe, Y., Sakai, T., Ménard, F., Aikawa, Y., Alves, F., Balucani, N., Bouvier, M., Caselli, P., Caux, E., Charnley, S., Choudhury, S., De Simone, M., Dulieu, F., Durán, A., Evans, L., Favre, C., Fedele, D., Feng, S., Fontani, F., Francis, L., Hama, T., Hanawa, T., Herbst, E., Hirota, T., Imai, M., Isella, A., Jiménez-Serra, I., Johnstone, D., Kahane, C., Lefloch, B., Loinard, L., Maureira, M. J., Mercimek, S., Miotello, A., Mori, S., Nakatani, R., Nomura, H., Oba, Y., Ohashi, S., Okoda, Y., Ospina-Zamudio, J., Oya, Y., Pineda, J., Podio, L., Rimola, A., Cox, D. Segura, Shirley, Y., Taquet, V., Testi, L., Vastel, C., Viti, S., Watanabe, N., Witzel, A., Xue, C., Zhang, Y., Zhao, B., Yamamoto, S., Bianchi, E., Chandler, C. J., Ceccarelli, C., Codella, C., Sakai, N., López-Sepulcre, A., Maud, L. T., Moellenbrock, G., Svoboda, B., Watanabe, Y., Sakai, T., Ménard, F., Aikawa, Y., Alves, F., Balucani, N., Bouvier, M., Caselli, P., Caux, E., Charnley, S., Choudhury, S., De Simone, M., Dulieu, F., Durán, A., Evans, L., Favre, C., Fedele, D., Feng, S., Fontani, F., Francis, L., Hama, T., Hanawa, T., Herbst, E., Hirota, T., Imai, M., Isella, A., Jiménez-Serra, I., Johnstone, D., Kahane, C., Lefloch, B., Loinard, L., Maureira, M. J., Mercimek, S., Miotello, A., Mori, S., Nakatani, R., Nomura, H., Oba, Y., Ohashi, S., Okoda, Y., Ospina-Zamudio, J., Oya, Y., Pineda, J., Podio, L., Rimola, A., Cox, D. Segura, Shirley, Y., Taquet, V., Testi, L., Vastel, C., Viti, S., Watanabe, N., Witzel, A., Xue, C., Zhang, Y., Zhao, B., and Yamamoto, S.

Abstract

The study of hot corinos in Solar-like protostars has been so far mostly limited to the Class 0 phase, hampering our understanding of their origin and evolution. In addition, recent evidence suggests that planet formation starts already during Class I phase, which, therefore, represents a crucial step in the future planetary system chemical composition. Hence, the study of hot corinos in Class I protostars has become of paramount importance. Here we report the discovery of a hot corino towards the prototypical Class I protostar L1551 IRS5, obtained within the ALMA Large Program FAUST. We detected several lines from methanol and its isopotologues ($^{13}$CH$_{\rm 3}$OH and CH$_{\rm 2}$DOH), methyl formate and ethanol. Lines are bright toward the north component of the IRS5 binary system, and a possible second hot corino may be associated with the south component. The methanol lines non-LTE analysis constrains the gas temperature ($\sim$100 K), density ($\geq$1.5$\times$10$^{8}$ cm$^{-3}$), and emitting size ($\sim$10 au in radius). All CH$_{\rm 3}$OH and $^{13}$CH$_{\rm 3}$OH lines are optically thick, preventing a reliable measure of the deuteration. The methyl formate and ethanol relative abundances are compatible with those measured in Class 0 hot corinos. Thus, based on the present work, little chemical evolution from Class 0 to I hot corinos occurs., Comment: 6 pages, 2 figures

Published
2020
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42. Hunting for hot corinos and WCCC sources in the OMC-2/3 filament

Author

Bouvier, M., López-Sepulcre, A., Ceccarelli, C., Kahane, C., Imai, M., Sakai, N., Yamamoto, S., Dagdigian, P. J., Bouvier, M., López-Sepulcre, A., Ceccarelli, C., Kahane, C., Imai, M., Sakai, N., Yamamoto, S., and Dagdigian, P. J.

Abstract

Context: Solar-like protostars are known to be chemically rich, but it is not yet clear how much their chemical composition can vary and why. So far, two chemically distinct types of Solar-like protostars have been identified: hot corinos, which are enriched in interstellar Complex Organic Molecules (iCOMs), such as methanol (CH$_3$OH) or dimethyl ether (CH$_3$OCH$_3$), and Warm Carbon Chain Chemistry (WCCC) objects, which are enriched in carbon chain molecules, such as butadiynyl (C$_4$H) or ethynyl radical (CCH). However, none of these have been studied so far in environments similar to that in which our Sun was born, that is, one that is close to massive stars. Aims: In this work, we search for hot corinos and WCCC objects in the closest analogue to the Sun's birth environment, the Orion Molecular Cloud 2/3 (OMC-2/3) filament located in the Orion A molecular cloud. Methods: We obtained single-dish observations of CCH and CH$_3$OH line emission towards nine Solar-like protostars in this region. As in other, similar studies of late, we used the [CCH]/[CH$_3$OH] abundance ratio in order to determine the chemical nature of our protostar sample. Results: Unexpectedly, we found that the observed methanol and ethynyl radical emission (over a few thousands au scale) does not seem to originate from the protostars but rather from the parental cloud and its photo-dissociation region, illuminated by the OB stars of the region. Conclusions: Our results strongly suggest that caution should be taken before using [CCH]/[CH$_3$OH] from single-dish observations as an indicator of the protostellar chemical nature and that there is a need for other tracers or high angular resolution observations for probing the inner protostellar layers., Comment: A&A, in press, 15 pages, 10 figures, 1 appendice (13 pages, 9 figures)

Published
2020
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43. Seeds of Life in Space (SOLIS).VII. Discovery of a cold dense methanol blob toward the L1521F VeLLO system

Author

Favre, C., Vastel, C., Jimenez-Serra, I., Quénard, D., Caselli, P., Ceccarelli, C., Chacón-Tanarro, A., Fontani, F., Holdship, J., Oya, Y., Punanova, A., Sakai, N., Spezzano, S., Yamamoto, S., Neri, R., López-Sepulcre, A., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Codella, C., Caux, E., De Simone, M., Romero, J. Enrique, Dulieu, F., Feng, S., Al-Edhari, A. Jaber, Lefloch, B., Ospina-Zamudio, J., Pineda, J., Podio, L., Rimola, A., Segura-Cox, D., Sims, I. R., Taquet, V., Testi, L., Theulé, P., Ugliengo, P., Vasyunin, A. I., Vazart, F., Viti, S., Witzel, A., Favre, C., Vastel, C., Jimenez-Serra, I., Quénard, D., Caselli, P., Ceccarelli, C., Chacón-Tanarro, A., Fontani, F., Holdship, J., Oya, Y., Punanova, A., Sakai, N., Spezzano, S., Yamamoto, S., Neri, R., López-Sepulcre, A., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Codella, C., Caux, E., De Simone, M., Romero, J. Enrique, Dulieu, F., Feng, S., Al-Edhari, A. Jaber, Lefloch, B., Ospina-Zamudio, J., Pineda, J., Podio, L., Rimola, A., Segura-Cox, D., Sims, I. R., Taquet, V., Testi, L., Theulé, P., Ugliengo, P., Vasyunin, A. I., Vazart, F., Viti, S., and Witzel, A.

Abstract

The SOLIS (Seeds Of Life In Space) IRAM/NOEMA Large Program aims at studying a set of crucial complex organic molecules in a sample of sources, with well-known physical structure, covering the various phases of Solar-type star formation. One representative object of the transition from the prestellar core to the protostar phases has been observed toward the Very Low Luminosity Object (VeLLO) called L1521F. This type of source is important to study to make the link between prestellar cores and Class 0 sources and also to constrain the chemical evolution during the process of star formation. Two frequency windows (81.6-82.6 GHz and 96.65-97.65 GHz) were used to observe the emission from several complex organics toward the L1521F VeLLO. Only 2 transitions of methanol (A+, E2) have been detected in the narrow window centered at 96.7 GHz (with an upper limit on E1) in a very compact emission blob (~7'' corresponding to ~1000au) toward the NE of the L1521F protostar. The CS 2-1 transition is also detected within the WideX bandwidth. Consistently, with what has been found in prestellar cores, the methanol emission appears ~1000au away from the dust peak. The location of the methanol blob coincides with one of the filaments previously reported in the literature. The Tex of the gas inferred from methanol is (10$\pm$2) K, while the H2 gas density (estimated from the detected CS 2-1 emission and previous CS 5-4 ALMA obs.) is a factor >25 higher than the density in the surrounding environment (n(H2) >10$^{7}$ cm$^{-3}$). From its compactness, low excitation temperature and high gas density, we suggest that the methanol emission detected with NOEMA is either a cold and dense shock-induced blob, recently formed ($\leq$ few hundred years) by infalling gas or a cold and dense fragment that may have just been formed as a result of the intense gas dynamics found within the L1521F VeLLO system., Comment: 11 pages, 7 figures, 3 tables, accepted for publication by A&A

Published
2020
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44. Genetic and environmental variation in educational attainment: an individual-based analysis of 28 twin cohorts

Author

Silventoinen, K, Jelenkovic, A, Sund, R, Latvala, A, Honda, C, Inui, F, Tomizawa, R, Watanabe, M, Sakai, N, Rebato, E, Busjahn, A, Tyler, J, Hopper, JL, Ordonana, JR, Sanchez-Romera, JF, Colodro-Conde, L, Calais-Ferreira, L, Oliveira, VC, Ferreira, PH, Medda, E, Nistico, L, Toccaceli, V, Derom, CA, Vlietinck, RF, Loos, RJF, Siribaddana, SH, Hotopf, M, Sumathipala, A, Rijsdijk, F, Duncan, GE, Buchwald, D, Tynelius, P, Rasmussen, F, Tan, Q, Zhang, D, Pang, Z, Magnusson, PKE, Pedersen, NL, Aslan, AKD, Hwang, AE, Mack, TM, Krueger, RF, McGue, M, Pahlen, S, Brandt, I, Nilsen, TS, Harris, JR, Martin, NG, Medland, SE, Montgomery, GW, Willemsen, G, Bartels, M, van Beijsterveldt, CEM, Franz, CE, Kremen, WS, Lyons, MJ, Silberg, JL, Maes, HH, Kandler, C, Nelson, TL, Whitfield, KE, Corley, RP, Huibregtse, BM, Gatz, M, Butler, DA, Tarnoki, AD, Tarnoki, DL, Park, HA, Lee, J, Lee, SJ, Sung, J, Yokoyama, Y, Sorensen, TIA, Boomsma, D, Kaprio, J, Silventoinen, K, Jelenkovic, A, Sund, R, Latvala, A, Honda, C, Inui, F, Tomizawa, R, Watanabe, M, Sakai, N, Rebato, E, Busjahn, A, Tyler, J, Hopper, JL, Ordonana, JR, Sanchez-Romera, JF, Colodro-Conde, L, Calais-Ferreira, L, Oliveira, VC, Ferreira, PH, Medda, E, Nistico, L, Toccaceli, V, Derom, CA, Vlietinck, RF, Loos, RJF, Siribaddana, SH, Hotopf, M, Sumathipala, A, Rijsdijk, F, Duncan, GE, Buchwald, D, Tynelius, P, Rasmussen, F, Tan, Q, Zhang, D, Pang, Z, Magnusson, PKE, Pedersen, NL, Aslan, AKD, Hwang, AE, Mack, TM, Krueger, RF, McGue, M, Pahlen, S, Brandt, I, Nilsen, TS, Harris, JR, Martin, NG, Medland, SE, Montgomery, GW, Willemsen, G, Bartels, M, van Beijsterveldt, CEM, Franz, CE, Kremen, WS, Lyons, MJ, Silberg, JL, Maes, HH, Kandler, C, Nelson, TL, Whitfield, KE, Corley, RP, Huibregtse, BM, Gatz, M, Butler, DA, Tarnoki, AD, Tarnoki, DL, Park, HA, Lee, J, Lee, SJ, Sung, J, Yokoyama, Y, Sorensen, TIA, Boomsma, D, and Kaprio, J

Abstract

We investigated the heritability of educational attainment and how it differed between birth cohorts and cultural-geographic regions. A classical twin design was applied to pooled data from 28 cohorts representing 16 countries and including 193,518 twins with information on educational attainment at 25 years of age or older. Genetic factors explained the major part of individual differences in educational attainment (heritability: a2 = 0.43; 0.41-0.44), but also environmental variation shared by co-twins was substantial (c2 = 0.31; 0.30-0.33). The proportions of educational variation explained by genetic and shared environmental factors did not differ between Europe, North America and Australia, and East Asia. When restricted to twins 30 years or older to confirm finalized education, the heritability was higher in the older cohorts born in 1900-1949 (a2 = 0.44; 0.41-0.46) than in the later cohorts born in 1950-1989 (a2 = 0.38; 0.36-0.40), with a corresponding lower influence of common environmental factors (c2 = 0.31; 0.29-0.33 and c2 = 0.34; 0.32-0.36, respectively). In conclusion, both genetic and environmental factors shared by co-twins have an important influence on individual differences in educational attainment. The effect of genetic factors on educational attainment has decreased from the cohorts born before to those born after the 1950s.

Published
2020

45. Seeds of Life in Space (SOLIS): VI. Chemical evolution of sulfuretted species along the outflows driven by the low-mass protostellar binary NGC 1333-IRAS4A

Author

Taquet, V., Codella, C., De Simone, M., López-Sepulcre, A., Pineda, J. E., Segura-Cox, D., Ceccarelli, C., Caselli, P., Gusdorf, A., Persson, M. V., Alves, F., Caux, E., Favre, C., Fontani, F., Neri, R., Oya, Y., Sakai, N., Vastel, C., Yamamoto, S., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Chacón-Tanarro, A., Dulieu, F., Enrique-Romero, J., Feng, S., Holdship, J., Lefloch, B., Jaber, Al-Edhari, A., Jiménez-Serra, I., Kahane, C., Lattanzi, V., Ospina-Zamudio, J., Podio, L., Punanova, A., Rimola, A., Sims, I. R., Spezzano, S., Testi, L., Theulé, P., Ugliengo, P., Vasyunin, A. I., Vazart, F., Viti, S., Witzel, A., Taquet, V., Codella, C., De Simone, M., López-Sepulcre, A., Pineda, J. E., Segura-Cox, D., Ceccarelli, C., Caselli, P., Gusdorf, A., Persson, M. V., Alves, F., Caux, E., Favre, C., Fontani, F., Neri, R., Oya, Y., Sakai, N., Vastel, C., Yamamoto, S., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Chacón-Tanarro, A., Dulieu, F., Enrique-Romero, J., Feng, S., Holdship, J., Lefloch, B., Jaber, Al-Edhari, A., Jiménez-Serra, I., Kahane, C., Lattanzi, V., Ospina-Zamudio, J., Podio, L., Punanova, A., Rimola, A., Sims, I. R., Spezzano, S., Testi, L., Theulé, P., Ugliengo, P., Vasyunin, A. I., Vazart, F., Viti, S., and Witzel, A.

Abstract

Context. Low-mass protostars drive powerful molecular outflows that can be observed with millimetre and submillimetre telescopes. Various sulfuretted species are known to be bright in shocks and could be used to infer the physical and chemical conditions throughout the observed outflows. Aims. The evolution of sulfur chemistry is studied along the outflows driven by the NGC 1333-IRAS4A protobinary system located in the Perseus cloud to constrain the physical and chemical processes at work in shocks. Methods. We observed various transitions from OCS, CS, SO, and SO2 towards NGC 1333-IRAS4A in the 1.3, 2, and 3 mm bands using the IRAM NOrthern Extended Millimeter Array and we interpreted the observations through the use of the Paris-Durham shock model. Results. The targeted species clearly show different spatial emission along the two outflows driven by IRAS4A. OCS is brighter on small and large scales along the south outflow driven by IRAS4A1, whereas SO2 is detected rather along the outflow driven by IRAS4A2 that is extended along the north east-south west direction. SO is detected at extremely high radial velocity up to + 25 km s-1 relative to the source velocity, clearly allowing us to distinguish the two outflows on small scales. Column density ratio maps estimated from a rotational diagram analysis allowed us to confirm a clear gradient of the OCS/SO2 column density ratio between the IRAS4A1 and IRAS4A2 outflows. Analysis assuming non Local Thermodynamic Equilibrium of four SO2 transitions towards several SiO emission peaks suggests that the observed gas should be associated with densities higher than 105 cm-3 and relatively warm (T > 100 K) temperatures in most cases. Conclusions. The observed chemical differentiation between the two outflows of the IRAS4A system could be explained by a different chemical history. The outflow driven by IRAS4A1 is likely younger and more enriched in species initially formed in interstellar ices, such as OCS, and recently sputter

Published
2020

46. Seeds of Life in Space (SOLIS): VII. Discovery of a cold dense methanol blob toward the L1521F VeLLO system

Author

Favre, C., Vastel, C., Jimenez-Serra, I., Quénard, D., Caselli, P., Ceccarelli, C., Chacón-Tanarro, A., Fontani, F., Holdship, J., Oya, Y., Punanova, A., Sakai, N., Spezzano, S., Yamamoto, S., Neri, R., López-Sepulcre, A., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Codella, C., Caux, E., De, Simone, M., Enrique, Romero, J., Dulieu, F., Feng, S., Jaber, Al-Edhari, A., Lefloch, B., Ospina-Zamudio, J., Pineda, J., Podio, L., Rimola, A., Segura-Cox, D., Sims, I. R., Taquet, V., Testi, L., Theulé, P., Ugliengo, P., Vasyunin, A. I., Vazart, F., Viti, S., Witzel, A., Favre, C., Vastel, C., Jimenez-Serra, I., Quénard, D., Caselli, P., Ceccarelli, C., Chacón-Tanarro, A., Fontani, F., Holdship, J., Oya, Y., Punanova, A., Sakai, N., Spezzano, S., Yamamoto, S., Neri, R., López-Sepulcre, A., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Codella, C., Caux, E., De, Simone, M., Enrique, Romero, J., Dulieu, F., Feng, S., Jaber, Al-Edhari, A., Lefloch, B., Ospina-Zamudio, J., Pineda, J., Podio, L., Rimola, A., Segura-Cox, D., Sims, I. R., Taquet, V., Testi, L., Theulé, P., Ugliengo, P., Vasyunin, A. I., Vazart, F., Viti, S., and Witzel, A.

Abstract

Aims. The Seeds Of Life In Space IRAM/NOEMA large program aims at studying a set of crucial complex organic molecules in a sample of sources with a well-known physical structure that covers the various phases of solar-type star formation. One representative object of the transition from the prestellar core to the protostar phases has been observed toward the very low luminosity object (VeLLO) L1521F. This type of source is important to study to link prestellar cores and Class 0 sources and also to constrain the chemical evolution during the process of star formation. Methods. Two frequency windows (81.6-82.6 GHz and 96.65-97.65 GHz) were used to observe the emission from several complex organics toward the L1521F VeLLO. These setups cover transitions of ketene (H2CCO), propyne (CH3CCH), formamide (NH2CHO), methoxy (CH3O), methanol (CH3OH), dimethyl ether (CH3OCH3), and methyl formate (HCOOCH3). Results. Only two transitions of methanol (A+, E2) have been detected in the narrow window centered at 96.7 GHz (with an upper limit on E1) in a very compact emission blob (∼7″ corresponding to ∼1000 au) toward the northeast of the L1521F protostar. The CS 2-1 transition is also detected within theWideX bandwidth. Consistently with what has been found in prestellar cores, the methanol emission appears ∼1000 au away from the dust peak. The location of the methanol blob coincides with one of the filaments that have previously been reported in the literature. The excitation temperature of the gas inferred from methanol is (10 ± 2) K, while the H2 gas density (estimated from the detected CS 2-1 emission and previous CS 5-4 ALMA observations) is a factor >25 higher than the density in the surrounding environment (n(H2) ≥ 107 cm-3). Conclusions. Based on its compactness, low excitation temperature, and high gas density, we suggest that the methanol emission detected with NOEMA is (i) either a cold and dense shock-induced blob that formed recently (≤ a few hundred years) by infal

Published
2020

47. FAUST I. The hot corino at the heart of the prototypical Class I protostar L1551 IRS5

Author

Bianchi, E., Chandler, C. J., Ceccarelli, C., Codella, C., Sakai, N., López-Sepulcre, A., Maud, L. T., Moellenbrock, G., Svoboda, B., Watanabe, Y., Sakai, T., Ménard, F., Aikawa, Y., Alves, F., Balucani, N., Bouvier, M., Caselli, P., Caux, E., Charnley, S., Choudhury, S., De Simone, M., Dulieu, F., Durán, A., Evans, L., Favre, C., Fedele, D., Feng, S., Fontani, F., Francis, L., Hama, T., Hanawa, T., Herbst, E., Hirota, T., Imai, M., Isella, A., Jiménez-Serra, I., Johnstone, D., Kahane, C., Lefloch, B., Loinard, L., Maureira, M. J., Mercimek, S., Miotello, A., Mori, S., Nakatani, R., Nomura, H., Oba, Y., Ohashi, S., Okoda, Y., Ospina-Zamudio, J., Oya, Y., Pineda, J., Podio, L., Rimola, A., Cox, D. Segura, Shirley, Y., Taquet, V., Testi, L., Vastel, C., Viti, S., Watanabe, N., Witzel, A., Xue, C., Zhang, Y., Zhao, B., Yamamoto, S., Bianchi, E., Chandler, C. J., Ceccarelli, C., Codella, C., Sakai, N., López-Sepulcre, A., Maud, L. T., Moellenbrock, G., Svoboda, B., Watanabe, Y., Sakai, T., Ménard, F., Aikawa, Y., Alves, F., Balucani, N., Bouvier, M., Caselli, P., Caux, E., Charnley, S., Choudhury, S., De Simone, M., Dulieu, F., Durán, A., Evans, L., Favre, C., Fedele, D., Feng, S., Fontani, F., Francis, L., Hama, T., Hanawa, T., Herbst, E., Hirota, T., Imai, M., Isella, A., Jiménez-Serra, I., Johnstone, D., Kahane, C., Lefloch, B., Loinard, L., Maureira, M. J., Mercimek, S., Miotello, A., Mori, S., Nakatani, R., Nomura, H., Oba, Y., Ohashi, S., Okoda, Y., Ospina-Zamudio, J., Oya, Y., Pineda, J., Podio, L., Rimola, A., Cox, D. Segura, Shirley, Y., Taquet, V., Testi, L., Vastel, C., Viti, S., Watanabe, N., Witzel, A., Xue, C., Zhang, Y., Zhao, B., and Yamamoto, S.

Abstract

The study of hot corinos in Solar-like protostars has been so far mostly limited to the Class 0 phase, hampering our understanding of their origin and evolution. In addition, recent evidence suggests that planet formation starts already during Class I phase, which, therefore, represents a crucial step in the future planetary system chemical composition. Hence, the study of hot corinos in Class I protostars has become of paramount importance. Here we report the discovery of a hot corino towards the prototypical Class I protostar L1551 IRS5, obtained within the ALMA Large Program FAUST. We detected several lines from methanol and its isopotologues ($^{13}$CH$_{\rm 3}$OH and CH$_{\rm 2}$DOH), methyl formate and ethanol. Lines are bright toward the north component of the IRS5 binary system, and a possible second hot corino may be associated with the south component. The methanol lines non-LTE analysis constrains the gas temperature ($\sim$100 K), density ($\geq$1.5$\times$10$^{8}$ cm$^{-3}$), and emitting size ($\sim$10 au in radius). All CH$_{\rm 3}$OH and $^{13}$CH$_{\rm 3}$OH lines are optically thick, preventing a reliable measure of the deuteration. The methyl formate and ethanol relative abundances are compatible with those measured in Class 0 hot corinos. Thus, based on the present work, little chemical evolution from Class 0 to I hot corinos occurs., Comment: 6 pages, 2 figures

Published
2020
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48. Hunting for hot corinos and WCCC sources in the OMC-2/3 filament

Author

Bouvier, M., López-Sepulcre, A., Ceccarelli, C., Kahane, C., Imai, M., Sakai, N., Yamamoto, S., Dagdigian, P. J., Bouvier, M., López-Sepulcre, A., Ceccarelli, C., Kahane, C., Imai, M., Sakai, N., Yamamoto, S., and Dagdigian, P. J.

Abstract

Context: Solar-like protostars are known to be chemically rich, but it is not yet clear how much their chemical composition can vary and why. So far, two chemically distinct types of Solar-like protostars have been identified: hot corinos, which are enriched in interstellar Complex Organic Molecules (iCOMs), such as methanol (CH$_3$OH) or dimethyl ether (CH$_3$OCH$_3$), and Warm Carbon Chain Chemistry (WCCC) objects, which are enriched in carbon chain molecules, such as butadiynyl (C$_4$H) or ethynyl radical (CCH). However, none of these have been studied so far in environments similar to that in which our Sun was born, that is, one that is close to massive stars. Aims: In this work, we search for hot corinos and WCCC objects in the closest analogue to the Sun's birth environment, the Orion Molecular Cloud 2/3 (OMC-2/3) filament located in the Orion A molecular cloud. Methods: We obtained single-dish observations of CCH and CH$_3$OH line emission towards nine Solar-like protostars in this region. As in other, similar studies of late, we used the [CCH]/[CH$_3$OH] abundance ratio in order to determine the chemical nature of our protostar sample. Results: Unexpectedly, we found that the observed methanol and ethynyl radical emission (over a few thousands au scale) does not seem to originate from the protostars but rather from the parental cloud and its photo-dissociation region, illuminated by the OB stars of the region. Conclusions: Our results strongly suggest that caution should be taken before using [CCH]/[CH$_3$OH] from single-dish observations as an indicator of the protostellar chemical nature and that there is a need for other tracers or high angular resolution observations for probing the inner protostellar layers., Comment: A&A, in press, 15 pages, 10 figures, 1 appendice (13 pages, 9 figures)

Published
2020
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49. Seeds of Life in Space (SOLIS).VII. Discovery of a cold dense methanol blob toward the L1521F VeLLO system

Author

Favre, C., Vastel, C., Jimenez-Serra, I., Quénard, D., Caselli, P., Ceccarelli, C., Chacón-Tanarro, A., Fontani, F., Holdship, J., Oya, Y., Punanova, A., Sakai, N., Spezzano, S., Yamamoto, S., Neri, R., López-Sepulcre, A., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Codella, C., Caux, E., De Simone, M., Romero, J. Enrique, Dulieu, F., Feng, S., Al-Edhari, A. Jaber, Lefloch, B., Ospina-Zamudio, J., Pineda, J., Podio, L., Rimola, A., Segura-Cox, D., Sims, I. R., Taquet, V., Testi, L., Theulé, P., Ugliengo, P., Vasyunin, A. I., Vazart, F., Viti, S., Witzel, A., Favre, C., Vastel, C., Jimenez-Serra, I., Quénard, D., Caselli, P., Ceccarelli, C., Chacón-Tanarro, A., Fontani, F., Holdship, J., Oya, Y., Punanova, A., Sakai, N., Spezzano, S., Yamamoto, S., Neri, R., López-Sepulcre, A., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Codella, C., Caux, E., De Simone, M., Romero, J. Enrique, Dulieu, F., Feng, S., Al-Edhari, A. Jaber, Lefloch, B., Ospina-Zamudio, J., Pineda, J., Podio, L., Rimola, A., Segura-Cox, D., Sims, I. R., Taquet, V., Testi, L., Theulé, P., Ugliengo, P., Vasyunin, A. I., Vazart, F., Viti, S., and Witzel, A.

Abstract

The SOLIS (Seeds Of Life In Space) IRAM/NOEMA Large Program aims at studying a set of crucial complex organic molecules in a sample of sources, with well-known physical structure, covering the various phases of Solar-type star formation. One representative object of the transition from the prestellar core to the protostar phases has been observed toward the Very Low Luminosity Object (VeLLO) called L1521F. This type of source is important to study to make the link between prestellar cores and Class 0 sources and also to constrain the chemical evolution during the process of star formation. Two frequency windows (81.6-82.6 GHz and 96.65-97.65 GHz) were used to observe the emission from several complex organics toward the L1521F VeLLO. Only 2 transitions of methanol (A+, E2) have been detected in the narrow window centered at 96.7 GHz (with an upper limit on E1) in a very compact emission blob (~7'' corresponding to ~1000au) toward the NE of the L1521F protostar. The CS 2-1 transition is also detected within the WideX bandwidth. Consistently, with what has been found in prestellar cores, the methanol emission appears ~1000au away from the dust peak. The location of the methanol blob coincides with one of the filaments previously reported in the literature. The Tex of the gas inferred from methanol is (10$\pm$2) K, while the H2 gas density (estimated from the detected CS 2-1 emission and previous CS 5-4 ALMA obs.) is a factor >25 higher than the density in the surrounding environment (n(H2) >10$^{7}$ cm$^{-3}$). From its compactness, low excitation temperature and high gas density, we suggest that the methanol emission detected with NOEMA is either a cold and dense shock-induced blob, recently formed ($\leq$ few hundred years) by infalling gas or a cold and dense fragment that may have just been formed as a result of the intense gas dynamics found within the L1521F VeLLO system., Comment: 11 pages, 7 figures, 3 tables, accepted for publication by A&A

Published
2020
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50. Seeds of Life in Space (SOLIS): VII. Discovery of a cold dense methanol blob toward the L1521F VeLLO system

Author

Favre, C., Vastel, C., Jiménez-Serra, Izaskun, Quénard, D., Caselli, P., Ceccarelli, C., Chacón-Tanarro, A., Fontani, F., Holdship, Jonathan, Oya, Y., Punanova, A., Sakai, N., Spezzano, S., Yamamoto, S., Neri, Roberto, López-Sepulcre, A., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Codella, Claudio, Caux, E., De Simone, M., Enrique Romero, J., Dulieu, F., Feng, S., Jaber Al-Edhari, A., Lefloch, Bertrand, Ospina-Zamudio, J., Pineda, J., Podio, L., Rimola, Albert, Segura-Cox, Dominique, Sims, I.R., Taquet, V., Testi, L., Theulé, Patrice, Ugliengo, Piero, Vasyunin, Anton I., Vazart, F., Viti, S., Witzel, A., Favre, C., Vastel, C., Jiménez-Serra, Izaskun, Quénard, D., Caselli, P., Ceccarelli, C., Chacón-Tanarro, A., Fontani, F., Holdship, Jonathan, Oya, Y., Punanova, A., Sakai, N., Spezzano, S., Yamamoto, S., Neri, Roberto, López-Sepulcre, A., Alves, F., Bachiller, R., Balucani, N., Bianchi, E., Bizzocchi, L., Codella, Claudio, Caux, E., De Simone, M., Enrique Romero, J., Dulieu, F., Feng, S., Jaber Al-Edhari, A., Lefloch, Bertrand, Ospina-Zamudio, J., Pineda, J., Podio, L., Rimola, Albert, Segura-Cox, Dominique, Sims, I.R., Taquet, V., Testi, L., Theulé, Patrice, Ugliengo, Piero, Vasyunin, Anton I., Vazart, F., Viti, S., and Witzel, A.

Abstract

Aims. The Seeds Of Life In Space IRAM/NOEMA large program aims at studying a set of crucial complex organic molecules in a sample of sources with a well-known physical structure that covers the various phases of solar-type star formation. One representative object of the transition from the prestellar core to the protostar phases has been observed toward the very low luminosity object (VeLLO) L1521F. This type of source is important to study to link prestellar cores and Class 0 sources and also to constrain the chemical evolution during the process of star formation. Methods. Two frequency windows (81.6-82.6 GHz and 96.65-97.65 GHz) were used to observe the emission from several complex organics toward the L1521F VeLLO. These setups cover transitions of ketene (HCCO), propyne (CHCCH), formamide (NHCHO), methoxy (CHO), methanol (CHOH), dimethyl ether (CHOCH), and methyl formate (HCOOCH). Results. Only two transitions of methanol (A, E) have been detected in the narrow window centered at 96.7 GHz (with an upper limit on E) in a very compact emission blob (∼7″ corresponding to ∼1000 au) toward the northeast of the L1521F protostar. The CS 2-1 transition is also detected within theWideX bandwidth. Consistently with what has been found in prestellar cores, the methanol emission appears ∼1000 au away from the dust peak. The location of the methanol blob coincides with one of the filaments that have previously been reported in the literature. The excitation temperature of the gas inferred from methanol is (10 ± 2) K, while the H gas density (estimated from the detected CS 2-1 emission and previous CS 5-4 ALMA observations) is a factor >25 higher than the density in the surrounding environment (n(H) ≥ 10 cm). Conclusions. Based on its compactness, low excitation temperature, and high gas density, we suggest that the methanol emission detected with NOEMA is (i) either a cold and dense shock-induced blob that formed recently (≤ a few hundred years) by infalling gas or (ii) a

Published
2020

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