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31 results on '"Pacucci, F."'

1. COSMOS-Web: The emergence of the Hubble Sequence

Author

Huertas-Company, M., Shuntov, M., Dong, Y., Walmsley, M., Ilbert, O., McCracken, H. J., Akins, H. B., Allen, N., Casey, C. M., Costantin, L., Daddi, E., Dekel, A., Franco, M., Garland, I. L., Géron, T., Gozaliasl, G., Hirschmann, M., Kartaltepe, J. S., Koekemoer, A. M., Lintott, C., Liu, D., Lucas, R., Masters, K., Pacucci, F., Paquereau, L., P'erez-Gonz'alez, P. G., Rhodes, J. D., Robertson, B. E., Simmons, B., Smethurst, R., Toft, S., and Yang, L.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Leveraging the wide area coverage of the COSMOS-Web survey, we quantify the abundance of different morphological types from $z\sim 7$ with unprecedented statistics and establish robust constraints on the epoch of emergence of the Hubble sequence. We measure the global (spheroids, disk-dominated, bulge-dominated, peculiar) and resolved (stellar bars) morphologies for about 400,000 galaxies down to F150W=27 using deep learning, representing a two-orders-of-magnitude increase over previous studies. We then provide reference Stellar Mass Functions (SMFs) of different morphologies between $z\sim 0.2$ and $z\sim 7$ and best-fit parameters to inform models of galaxy formation. All catalogs and data are made publicly available. (a)At redshift z > 4.5, the massive galaxy population ($\log M_*/M_\odot>10$) is dominated by disturbed morphologies (~70%) -- even in the optical rest frame -- and very compact objects (~30%) with effective radii smaller than ~500pc. This confirms that a significant fraction of the star formation at cosmic dawn occurs in very dense regions, although the stellar mass for these systems could be overestimated.(b)Galaxies with Hubble-type morphologies -- including bulge and disk-dominated galaxies -- arose rapidly around $z\sim 4$ and dominate the morphological diversity of massive galaxies as early as $z\sim 3$. (c)Using stellar bars as a proxy, we speculate that stellar disks in massive galaxies might have been common (>50%) among the star-forming population since cosmic noon ($z\sim2$-2.5) and formed as early as $z\sim 7$ (d)Massive quenched galaxies are predominantly bulge-dominated from z~4 onward, suggesting that morphological transformations briefly precede or are simultaneous to quenching mechanisms at the high-mass end. (e) Low-mass ($\log M_*/M_\odot<10$) quenched galaxies are typically disk-dominated, pointing to different quenching routes in the two ends of the stellar mass spectrum from cosmic dawn., Comment: subnmitted to A&A. Comments Welcome

Published
2025

2. Ultra High-Redshift or Closer-by, Dust-Obscured Galaxies? Deciphering the Nature of Faint, Previously Missed F200W-Dropouts in CEERS

Author

Gandolfi, G., Rodighiero, G., Bisigello, L., Grazian, A., Finkelstein, S. L., Dickinson, M., Castellano, M., Merlin, E., Calabrò, A., Papovich, C., Bianchetti, A., Bañados, E., Benotto, P., Buitrago, F., Daddi, E., Girardi, G., Giulietti, M., Hirschmann, M., Holwerda, B. W., Haro, P. Arrabal, Lapi, A., Lucas, R. A., Lyu, Y., Massardi, M., Pacucci, F., Pérez-González, P. G., Ronconi, T., Tarrasse, M., Wilkins, S., Vulcani, B., Yung, L. Y. A., Zavala, J. A., Backhaus, B., Bagley, M., Buat, V., Burgarella, D., Kartaltepe, J., Khusanova, Y., Kirkpatrick, A., Kocevski, D., Koekemoer, A. M., Lambrides, E., Pirzkal, N., and Yang, G.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The James Webb Space Telescope (JWST) is revolutionizing our understanding of the Universe by unveiling faint, near-infrared dropouts previously beyond our reach, ranging from exceptionally dusty sources to galaxies up to redshift $z \sim 14$. In this paper, we identify F200W-dropout objects in the Cosmic Evolution Early Release Science (CEERS) survey which are absent from existing catalogs. Our selection method can effectively identify obscured low-mass ($\log \text{M}_* \leq 9$) objects at $z \leq 6$, massive dust-rich sources up to $z \sim 12$, and ultra-high-redshift ($z > 15$) candidates. Primarily relying on NIRCam photometry from the latest CEERS data release and supplementing with Mid-Infrared/(sub-)mm data when available, our analysis pipeline combines multiple SED-fitting codes, star formation histories, and CosMix - a novel tool for astronomical stacking. Our work highlights three $215$, with best-fit masses compatible with $\Lambda$CDM and a standard baryons-to-star conversion efficiency. Their bi-modal redshift probability distributions suggest they could also be $z<1.5$ dwarf galaxies with extreme dust extinction. We also identify a strong line emitter galaxy at $z \sim 5$ mimicking the near-infrared emission of a $z \sim 13$ galaxy. Our sample holds promising candidates for future follow-ups. Confirming ultra high-redshift galaxies or lower-z dusty dwarfs will offer valuable insights into early galaxy formation, evolution with their central black holes and the nature of dark matter, and/or cosmic dust production mechanisms in low-mass galaxies, and will help us to understand degeneracies and contamination in high-z object searches., Comment: Submitted to Astronomy & Astrophysics

Published
2025

3. Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe

Author

Mascia, S., Pentericci, L., Llerena, M., Calabrò, A., Matthee, J., Flury, S., Pacucci, F., Jaskot, A., Amorín, R. O., Bhatawdekar, R., Castellano, M., Cleri, N., Costantin, L., Davis, K., Di Cesare, C., Dickinson, M., Fontana, A., Guo, Y., Giavalisco, M., Holwerda, B. W., Hu, W., Huertas-Company, M., Jung, Intae, Kartaltepe, J., Kashino, D., Koekemoer, Anton M., Lucas, R. A., Lotz, J., Napolitano, L., Jogee, S., and Wilkins, S.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Compact, star-forming galaxies with high star formation rate surface densities ($\Sigma_{\text{SFR}}$) are often efficient Lyman continuum (LyC) emitters at $z\leq 4.5$, likely as intense stellar feedback creates low-density channels that allow photons to escape. Irregular or disturbed morphologies, such as those resulting from mergers, can also facilitate LyC escape by creating anisotropic gas distributions. We investigate the influence of galaxy morphology on LyC production and escape at redshifts $5 \leq z \leq 7$ using observations from various \textit{James Webb Space Telescope} (JWST) surveys. Our sample consists of 436 sources, which are predominantly low-mass ($\sim 10^{8.15} M_\odot$), star-forming galaxies with ionizing photon efficiency ($\xi_{\rm ion}$) values consistent with canonical expectations. Since direct measurements of $f_{\rm esc}$ are not possible during the Epoch of Reionization (EoR), we predict $f_{\rm esc}$ for high-redshift galaxies by applying survival analysis to a subsample of LyC emitters from the Low-Redshift Lyman Continuum Survey (LzLCS), selected to be direct analogs of reionization-era galaxies. We find that these galaxies exhibit on average modest predicted escape fractions ($\sim 0.04$). Additionally, we assess the correlation between morphological features and LyC emission. Our findings indicate that neither $\xi_{\rm ion}$ nor the predicted $f_{\rm esc}$ values show a significant correlation with the presence of merger signatures. This suggests that in low-mass galaxies at $z \geq 5$, strong morphological disturbances are not the primary mechanism driving LyC emission and leakage. Instead, compactness and star formation activity likely play a more pivotal role in regulating LyC escape., Comment: Submitted to A&A

Published
2025

4. Evolution of the UV slope of galaxies at cosmic morning (z > 4): the properties of extremely blue galaxies

Author

Dottorini, D., Calabrò, A., Pentericci, L., Mascia, S., Llerena, M., Napolitano, L., Santini, P., Roberts-Borsani, G., Castellano, M., Amorín, R., Dickinson, M., Fontana, A., Hathi, N., Hirschmann, M., Koekemoer, A., Lucas, R. A., Merlin, E., Morales, A., Pacucci, F., Wilkins, S., Haro, P. Arrabal, Bagley, M., Finkelstein, S., Kartaltepe, J., Papovich, C., and Pirzkal, N.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present an analysis of the UV continuum slope, beta, using a sample of 733 galaxies selected from a mixture of JWST ERS/GTO/GO observational programs and with z > 4. We consider spectroscopic data obtained with the low resolution PRISM/CLEAR NIRSpec configuration. Studying the correlation of beta with M_UV we find a decreasing trend of beta = (-0.056 +- 0.017) M_UV - (3.01 +- 0.34), consistent with brighter galaxies having redder beta as found in previous works. However, analysing the trend in separate redshift bins, we find that at high redshift the relation becomes much flatter, consistent with a flat slope. Furthermore, we find that beta decreases with redshift with an evolution as beta = (-0.075 +- 0.010) z - (1.496 +- 0.056), consistent with most previous results that show a steepening of the spectra going at higher z. We then select a sample of galaxies with extremely blue slopes (beta < -2.6): such slopes are steeper than what is predicted by stellar evolution models, even for dust free, young, metal poor populations, when the contribution of nebular emission is included. We select 51 extremely blue galaxies (XBGs) and we investigate the possible physical origin of their steep slopes, comparing them to a sub-sample of redder galaxies (matched in redshift and M_UV). We find that XBGs have younger stellar populations, stronger ionization fields, lower dust attenuation, and lower but not pristine metallicity (~ 10% solar) compared to red galaxies. However, these properties alone cannot explain the extreme beta values. By using indirect inference of Lyman continuum escape, using the most recent models, we estimate escape fractions f_esc > 10% in at least 25% of XBGs, while all the red sources have smaller f_esc. A reduced nebular continuum contribution as due to either a high escape fraction or to a bursty star-formation history is likely the origin of the extremely blue slopes., Comment: Submitted to A&A (12 pages, 6 figures, and 2 tables)

Published
2024

5. The ionizing photon production efficiency of star-forming galaxies at $z\sim 4-10$

Author

Llerena, M., Pentericci, L., Napolitano, L., Mascia, S., Amorín, R., Calabrò, A., Castellano, M., Cleri, N. J., Giavalisco, M., Grogin, N. A., Hathi, N. P., Hirschmann, M., Koekemoer, A. M., Nanayakkara, T., Pacucci, F., Shen, L., Wilkins, S. M., Yoon, I., Yung, L. Y. A., Bhatawdekar, R., Lucas, R. A., Wang, X., Haro, P. Arrabal, Bagley, M. B., Finkelstein, S. L., Kartaltepe, J. S., Merlin, E., Papovich, C., and Pirzkal, N.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Investigating the ionizing emission of star-forming galaxies is critical to understanding their contribution to reionization and their impact on the surrounding environment. The number of ionizing photons available to reionize the intergalactic medium (IGM) depends not only on the abundance of galaxies but also on their efficiency in producing ionizing photons ($\xi_{ion}$). We aim to estimate the $\xi_{ion}$ using Balmer lines in a sample of 731 galaxies at $4\leq z \leq 10$ selected from different JWST surveys. We used the available HST and JWST photometry to perform a SED fitting in the sample to determine their physical properties. We used the BAGPIPES code and assumed a delayed exponential model for the star formation history. We used the NIRSpec spectra from prism or grating configurations to estimate Balmer luminosities and then constrained $\xi_{ion}$ values after dust correction. We find a mean value of 10$^{25.23}$Hz erg$^{-1}$ for $\xi_{ion}$ in the sample with an observed scatter of 0.42dex. We find an increase in the median values of $\xi_{ion}$ which confirms the redshift evolution of $\xi_{ion}$ found in other works. Regarding the relation with physical properties, we find a decrease of $\xi_{ion}$ with increasing stellar mass, indicating that low-mass galaxies are efficient producers of ionizing photons. We also find an increase of $\xi_{ion}$ with increasing specific star formation rate (sSFR) and increasing UV absolute magnitude, which indicates that faint galaxies and with high sSFR are also efficient producers. We also investigated the relation of $\xi_{ion}$ with the EW([OIII]$\lambda$5007) and find that galaxies with the higher EW([OIII]) are the more efficient producers of ionizing photons. Similarly, we find that galaxies with higher O32 ratios and lower gas-phase metallicities (based on the R23 calibration) show higher $\xi_{ion}$ values., Comment: Submitted to A&A. Comments are welcome

Published
2024

6. Spectroscopic confirmation of a dust-obscured, metal-rich dwarf galaxy at z~5

Author

Bisigello, L., Gandolfi, G., Feltre, A., Haro, P. Arrabal, Calabrò, A., Cleri, N. J., Costantin, L., Girardi, G., Giulietti, M., Grazian, A., Gruppioni, C., Hathi, N. P., Holwerda, B. W., Llerena, M., Lucas, R. A., Pacucci, F., Prandoni, I., Rodighiero, G., Seillé, L. -M., Wilkins, S. M., Bagley, M., Dickinson., M., Finkelstein, S. L., Kartaltepe, J., Koekemoer, A. M., Papovich, C., and Pirzkal, N.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present the first spectroscopic confirmation of a dust-obscured dwarf galaxy, CEERS-14821. The analysis is performed combining JWST NIRCam broad-band photometry and NIRSpec/PRISM spectroscopic data. From the detection of multiple rest-frame optical lines, we derive that CEERS-14821 is located at $z=4.883\pm0.003$. Moreover, from a secure detection of the $H_{\alpha}$ and $H_{\beta}$ we derived that the galaxy has a dust extinction ranging from Av=2.2 to Av=3.3, depending on the assumed reddening law. This value is extremely large given that we estimated a low stellar mass around log(M/Mo)=8.0-8.2. Moreover, using different metallicity tracers, we verify that the galaxy is also metal-rich, with 12+log(O/H)>8.3. This is well above the expectation from both the mass-metallicity relation and the fundamental mass-metalliticy relation. CEERS-14821 is going through a burst of star formation, there are no indications of a strong contribution from an active galactic nuclei (f(AGN)<0.5 with respect to the total dust luminosity). Based on the rest-frame optical images, this source has a size compatible with galaxies of similar stellar mass and redshift. Finally, with the current data, it seems that there are galaxies closely interacting with CEERS-14821., Comment: 15 pages, 12 figures. Accepted by A&A on the 13th of December 2024

Published
2024
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7. Physical properties of strong 1 < z < 3 Balmer and Paschen lines emitters observed with JWST

Author

Seillé, L. -M., Buat, V., Fernández, V., Boquien, M., Roehlly, Y., Boselli, A., Calabrò, A., Amorín, R. O., Backhaus, B. E., Burgarella, D., Cleri, N. J., Dickinson, M., Hathi, N. P., Holwerda, B. W., Koekemoer, A. M., Napolitano, L., Pacucci, F., Robertson, C., and Yung, L. Y. A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The ultraviolet continuum traces young stars while the near-infrared unveils older stellar populations and dust-obscured regions. Balmer emission lines provide insights on gas properties and young stellar objects but are highly affected by dust attenuation. The near-infrared Paschen lines suffer less dust attenuation and can be used to measure star formation rates (SFRs) in star-forming regions obscured by dust clouds. We select 13 sources between redshifts 1 and 3 observed with HST, JWST/NIRCam and NIRSpec based on the availability of at least one Balmer and one Paschen line with S/N > 5. With a newly-developed version of CIGALE, we fit their hydrogen line equivalent widths (EWs) and photometric data. We assess the impacts of the removal of spectroscopic data by comparing the quality of the fits of the spectro-photometric data to those with photometric data only. We compare the single (BC03) vs binary (BPASS) stellar populations models in the fitting process of spectro-photometric data. We derive the differential attenuation and explore different attenuation recipes by fitting spectro-photometric data with BC03. For each stellar model and for each input dataset (with and without EWs), we quantify the deviation on the SFRs and stellar masses from the "standard" choice. On average, the SFRs are overestimated and the stellar masses are underestimated when EWs are not included as input data. We find a major contribution of the H${\alpha}$ emission line to the broadband photometric measurements of our sources, and a trend of increasing contribution with specific SFR. Using the BPASS models has a significant impact on the derived SFRs and stellar masses. We show that a flexible attenuation recipe provides more accurate estimates of the dust attenuation parameters, especially the differential attenuation which agrees with the original value of Charlot & Fall (2000)., Comment: Accepted in Astronomy & Astrophysics, 19 pages, 15 figures

Published
2024
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8. The evolution of the SFR and Sigma-SFR of galaxies in cosmic morning (4 < z < 10)

Author

Calabrò, A., Pentericci, L., Santini, P., Ferrara, A., Llerena, M., Mascia, S., Napolitano, L., Yung, L. Y. A., Bisigello, L., Castellano, M., Cleri, N. J., Dekel, A., Dickinson, M., Franco, M., Giavalisco, M., Hirschmann, M., Holwerda, B. W., Koekemoer, A. M., Lucas, R. A., Pacucci, F., Pirzkal, N., Roberts-Borsani, G., Seillé, L. M., Tacchella, S., Wilkins, S., Amorín, R., Haro, P. Arrabal, Bagley, M. B., Finkelstein, S. L., Kartaltepe, J. S., and Papovich, C.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The galaxy integrated star-formation rate (SFR) surface density ($\Sigma_{\rm SFR}$) has been proposed as a valuable diagnostic of the mass accumulation in galaxies as being more tightly related to the physics of star-formation (SF) and stellar feedback than other SF indicators. In this paper, we assemble a statistical sample of 230 galaxies observed with JWST in the GLASS and CEERS spectroscopic surveys to estimate Balmer line based dust attenuations and SFRs, and UV rest-frame effective radii. We study the evolution of galaxy SFR and $\Sigma_{\rm SFR}$ in the first 1.5 Billion years of our Universe, finding that $\Sigma_{\rm SFR}$ is mildly increasing with redshift with a linear slope of $0.16 \pm 0.06$. We also explore the dependence of SFR and $\Sigma_{\rm SFR}$ on stellar mass, showing that a SF 'Main-Sequence' and a $\Sigma_{\rm SFR}$ `Main-Sequence' are in place out to z=10, with a similar slope compared to the same relations at lower redshifts. We find that the specific SFR (sSFR) and $\Sigma_{\rm SFR}$ are correlated with the [OIII]5007/[OII]3727 ratio and with indirect estimates of the escape fraction of Lyman continuum photons, hence they likely play an important role in the evolution of ionization conditions and in the escape of ionizing radiation. We also search for spectral outflow signatures in a subset of galaxies observed at high resolution, finding an outflow incidence of $2/11$ ($=20\%^{32\%}_{9\%}$) at $z<6$, but no evidence at $z>6$ ($<26\%$). Finally, we find a positive correlation between A$_V$ and $\Sigma_{\rm SFR}$, and a flat trend as a function of sSFR, indicating that there is no evidence of a drop of A$_V$ in extremely star-forming galaxies between z=4 and 10. This might be at odds with a dust-clearing outflow scenario, which might instead take place at redshifts $z\geq 10$, as suggested by some theoretical models., Comment: Accepted for publication in A&A ; 19 pages, 9 figures, 1 table. Compared to the previous version, we have corrected a typo in Fig. 5 (the x and y axis labels were inverted)

Published
2024
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9. ASTRO2020 White Paper: JWST: Probing the Epoch of Reionization with a Wide Field Time-Domain Survey

Author

Wang, L., Mould, J., Baade, D., Baron, E., Bromm, V., Chen, T. -W., Cooke, J., Fan, X., Foley, R., Fruchter, A., Gal-Yam, A., Heger, A., Hoeflich, P., Howell, D. A., Kashlinsky, A., Kim, A., Koekemoer, A., Mather, J., Mazzali, P., Pacucci, F., Patat, F., Pian, E., Perlmutter, S., Rest, A., Rubin, D., Sand, D., Stubbs, C., Suntzeff, N., Wang, X. -F., Whalen, D., Wheeler, J. C., and Yue, B.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

A major scientific goal of JWST is to probe the epoch of re-ionization of the Universe at z above 6, and up to 20 and beyond. At these redshifts, galaxies are just beginning to form and the observable objects are early black holes, supernovae, and cosmic infrared background. The JWST has the necessary sensitivity to observe these targets individually, but a public deep and wide science enabling survey in the wavelength range from 2-5 $\mu$m is needed to discover these black holes and supernovae and to cover the area large enough for cosmic infrared background to be reliably studied. This enabling survey will also discover a large number of other transients and enable sciences such as supernova cosmology up to z $\sim$ 5, star formation history at high redshift through supernova explosions, faint stellar objects in the Milky Way, and galaxy evolution up to z approaching 10. The results of this survey will also serve as an invaluable target feeder for the upcoming era of ELT and SKA., Comment: arXiv admin note: text overlap with arXiv:1710.07005

Published
2019

10. A First Transients Survey with JWST: the FLARE project

Author

Wang, Lifan, Baade, D., Baron, E., Bernard, S., Bromm, V., Brown, P., Clayton, G., Cooke, J., Croton, D., Curtin, C., Drout, M., Doi, M., Dominguez, I., Finkelstein, S., Gal-Yam, A., Geil, P., Heger, A., Hoeflich, P., Jian, J., Krisciunas, K., Koekemoer, A., Lunnan, R., Maeda, K., Maund, J., Modjaz, M., Mould, J., Nomoto, K., Nugent, P., Patat, F., Pacucci, F., Phillips, M., Rest, A., Regos, E., Sand, D., Sparks, B., Spyromilio, J., Staveley-Smith, L., Suntzeff, N., Uddin, S., Villarroel, B., Vinko, J., Whalen, D., Wheeler, J., Wood-Vasey, M., Yang, Y., and Yue, Bin

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

JWST was conceived and built to answer one of the most fundamental questions that humans can address empirically: "How did the Universe make its first stars?". Our First Lights At REionization (FLARE) project transforms the quest for the epoch of reionization from the static to the time domain. It targets the complementary question: "What happened to those first stars?". It will be answered by observations of the most luminous events: supernovae and accretion on to black holes formed by direct collapse from the primordial gas clouds. These transients provide direct constraints on star-formation rates (SFRs) and the truly initial Initial Mass Function (IMF), and they may identify possible stellar seeds of supermassive black holes (SMBHs). Furthermore, our knowledge of the physics of these events at ultra-low metallicity will be much expanded. JWST's unique capabilities will detect these most luminous and earliest cosmic messengers easily in fairly shallow observations. However, these events are very rare at the dawn of cosmic structure formation and so require large area coverage. Time domain astronomy can be advanced to an unprecedented depth by means of a shallow field of JWST reaching 27 mag AB in 2 and 4.4 microns over a field as large as 0.1 square degree visited multiple times each year. Such a survey may set strong constraints or detect massive Pop III SNe at redshifts beyond 10, pinpointing the redshift of the first stars, or at least their death. Based on our current knowledge of superluminous supernovae (SLSNe), such a survey will find one or more SLSNe at redshifts above 6 in five years and possibly several direct collapse black holes. Although JWST is not designed as a wide field survey telescope, we show that such a wide field survey is possible with JWST and is critical in addressing several of its key scientific goals.

Published
2017

11. The Brightest Ly$\alpha$ Emitter: Pop III or Black Hole?

Author

Pallottini, A., Ferrara, A., Pacucci, F., Gallerani, S., Salvadori, S., Schneider, R., Schaerer, D., Sobral, D., and Matthee, J.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

CR7 is the brightest $z=6.6 \, {\rm Ly}\alpha$ emitter (LAE) known to date, and spectroscopic follow-up by Sobral et al. (2015) suggests that CR7 might host Population (Pop) III stars. We examine this interpretation using cosmological hydrodynamical simulations. Several simulated galaxies show the same "Pop III wave" pattern observed in CR7. However, to reproduce the extreme CR7 ${\rm Ly}\alpha$/HeII1640 line luminosities ($L_{\rm \alpha/He II}$) a top-heavy IMF and a massive ($>10^{7}{\rm M}_{\odot}$) PopIII burst with age $<2$ Myr are required. Assuming that the observed properties of ${\rm Ly}\alpha$ and HeII emission are typical for Pop III, we predict that in the COSMOS/UDS/SA22 fields, 14 out of the 30 LAEs at $z=6.6$ with $L_{\alpha} >10^{43.3}{\rm erg}\,{\rm s}^{-1}$ should also host Pop III stars producing an observable $L_{\rm He II}>10^{42.7}{\rm erg}\,{\rm s}^{-1}$. As an alternate explanation, we explore the possibility that CR7 is instead powered by accretion onto a Direct Collapse Black Hole (DCBH). Our model predicts $L_{\alpha}$, $L_{\rm He II}$, and X-ray luminosities that are in agreement with the observations. In any case, the observed properties of CR7 indicate that this galaxy is most likely powered by sources formed from pristine gas. We propose that further X-ray observations can distinguish between the two above scenarios., Comment: 6 pages, 4 figures

Published
2015
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12. Evolution of the star formation rate and ΣSFR of galaxies at cosmic morning (4  <  z  <  10).

Author

Calabrò, A., Pentericci, L., Santini, P., Ferrara, A., Llerena, M., Mascia, S., Napolitano, L., Yung, L. Y. A., Bisigello, L., Castellano, M., Cleri, N. J., Dekel, A., Dickinson, M., Franco, M., Giavalisco, M., Hirschmann, M., Holwerda, B. W., Koekemoer, A. M., Lucas, R. A., and Pacucci, F.

Subjects
GALACTIC evolution, STELLAR mass, STELLAR evolution, GALACTIC redshift, GALAXY formation, REDSHIFT, STAR formation
Abstract

The galaxy-integrated star formation rate (SFR) surface density measurement (ΣSFR) has been proposed as a valuable diagnostic of the mass accumulation in galaxies given it is more tightly related to the physics of star formation and stellar feedback than other indicators. In this work, we assembled a statistical sample of 230 galaxies observed with JWST in the GLASS and CEERS spectroscopic surveys to estimate Balmer line-based dust attenuations and SFRs (i.e., from Hα, Hβ, and Hγ), along with the UV rest-frame effective radii. We studied the evolution of galaxy SFR and ΣSFR in the first 1.5 billion years of our Universe, from a redshift of z ∼ 4 to z ∼ 10. We found that ΣSFR is mildly increasing with redshift with a linear slope of 0.16 ± 0.06. We explored the dependence of SFR and ΣSFR on stellar mass, showing that a star-forming main sequence and a ΣSFR main sequence are present out to z = 10. This dependence exhibits a similar slope compared to the same relations at lower redshifts, but with a higher normalization. We find that the specific SFR (sSFR) and ΣSFR are correlated with the [O III] λ5007 Å/[O II] λ3727 Å ratio and with indirect estimates of the escape fraction of Lyman continuum photons; hence, they are likely to play an important role in the evolution of ionization conditions at higher redshifts and in the escape of ionizing radiation. We also searched for spectral outflow signatures in the Hα and [O III] emission lines in a subset of galaxies observed at high resolution (R = 2700) by the GLASS survey, finding an outflow incidence of 2/11 (=20%32%9%) = 20 % 9 % 32 % at z < 6, but no evidence at z > 6 (0/6, < 26%). Finally, we find a positive correlation between AV and ΣSFR, and a flat trend as a function of sSFR, indicating that there is no evidence of a drop in AV in extremely star-forming galaxies between z ∼ 4 and ∼10. This result might be at odds with a dust-clearing outflow scenario, which may instead take place at redshifts of z ≥ 10, as suggested by some theoretical models. [ABSTRACT FROM AUTHOR]

Published
2024
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13. The evolution of the SFR and $\Sigma_{SFR}$ of galaxies in cosmic morning ($4<z<10$)

Author

Calabrò, A., Pentericci, L., Santini, P., Ferrara, A., Llerena, M., Mascia, S., Napolitano, L., Yung, L. Y. A., Bisigello, L., Cleri, N. J., Dekel, A., Dickinson, M., Franco, M., Giavalisco, M., Hirschmann, M., Holwerda, B. W., Koekemoer, A. M., Lucas, R. A., Pacucci, F., Pirzkal, N., Roberts-Borsani, G., Seillé, L. M., Tacchella, S., Wilkins, S., Amorín, R., Haro, P. Arrabal, Bagley, M. B., Finkelstein, S. L., Kartaltepe, J. S., Papovich, C., Calabrò, A., Pentericci, L., Santini, P., Ferrara, A., Llerena, M., Mascia, S., Napolitano, L., Yung, L. Y. A., Bisigello, L., Cleri, N. J., Dekel, A., Dickinson, M., Franco, M., Giavalisco, M., Hirschmann, M., Holwerda, B. W., Koekemoer, A. M., Lucas, R. A., Pacucci, F., Pirzkal, N., Roberts-Borsani, G., Seillé, L. M., Tacchella, S., Wilkins, S., Amorín, R., Haro, P. Arrabal, Bagley, M. B., Finkelstein, S. L., Kartaltepe, J. S., and Papovich, C.

Abstract

The galaxy integrated star-formation rate (SFR) surface density ($\Sigma_{\rm SFR}$) has been proposed as a valuable diagnostic of the mass accumulation in galaxies as being more tightly related to the physics of star-formation (SF) and stellar feedback than other SF indicators. In this paper, we assemble a statistical sample of 230 galaxies observed with JWST in the GLASS and CEERS spectroscopic surveys to estimate Balmer line based dust attenuations and SFRs, and UV rest-frame effective radii. We study the evolution of galaxy SFR and $\Sigma_{\rm SFR}$ in the first 1.5 Billion years of our Universe, finding that $\Sigma_{\rm SFR}$ is mildly increasing with redshift with a linear slope of $0.16 \pm 0.06$. We also explore the dependence of SFR and $\Sigma_{\rm SFR}$ on stellar mass, showing that a SF 'Main-Sequence' and a $\Sigma_{\rm SFR}$ `Main-Sequence' are in place out to z=10, with a similar slope compared to the same relations at lower redshifts. We find that the specific SFR (sSFR) and $\Sigma_{\rm SFR}$ are correlated with the [OIII]5007/[OII]3727 ratio and with indirect estimates of the escape fraction of Lyman continuum photons, hence they likely play an important role in the evolution of ionization conditions and in the escape of ionizing radiation. We also search for spectral outflow signatures in a subset of galaxies observed at high resolution, finding an outflow incidence of $2/11$ ($=20\%^{32\%}_{9\%}$) at $z<6$, but no evidence at $z>6$ ($<26\%$). Finally, we find a positive correlation between A$_V$ and $\Sigma_{\rm SFR}$, and a flat trend as a function of sSFR, indicating that there is no evidence of a drop of A$_V$ in extremely star-forming galaxies between z=4 and 10. This might be at odds with a dust-clearing outflow scenario, which might instead take place at redshifts $z\geq 10$, as suggested by some theoretical models., Comment: Submitted to A&A ; 17 pages, 9 figures, 1 table

Published
2024

14. Cosmology with the Laser Interferometer Space Antenna

Author

Auclair, P, Bacon, D, Baker, T, Barreiro, T, Bartolo, N, Belgacem, E, Bellomo, N, Ben-Dayan, I, Bertacca, D, Besancon, M, Blanco-Pillado, J, Blas, D, Boileau, G, Calcagni, G, Caldwell, R, Caprini, C, Carbone, C, Chang, C, Chen, H, Christensen, N, Clesse, S, Comelli, D, Congedo, G, Contaldi, C, Crisostomi, M, Croon, D, Cui, Y, Cusin, G, Cutting, D, Dalang, C, De Luca, V, Pozzo, W, Desjacques, V, Dimastrogiovanni, E, Dorsch, G, Ezquiaga, J, Fasiello, M, Figueroa, D, Flauger, R, Franciolini, G, Frusciante, N, Fumagalli, J, Garcia-Bellido, J, Gould, O, Holz, D, Iacconi, L, Jain, R, Jenkins, A, Jinno, R, Joana, C, Karnesis, N, Konstandin, T, Koyama, K, Kozaczuk, J, Kuroyanagi, S, Laghi, D, Lewicki, M, Lombriser, L, Madge, E, Maggiore, M, Malhotra, A, Mancarella, M, Mandic, V, Mangiagli, A, Matarrese, S, Mazumdar, A, Mukherjee, S, Musco, I, Nardini, G, No, J, Papanikolaou, T, Peloso, M, Pieroni, M, Pilo, L, Raccanelli, A, Renaux-Petel, S, Renzini, A, Ricciardone, A, Riotto, A, Romano, J, Rollo, R, Pol, A, Morales, E, Sakellariadou, M, Saltas, I, Scalisi, M, Schmitz, K, Schwaller, P, Sergijenko, O, Servant, G, Simakachorn, P, Sorbo, L, Sousa, L, Speri, L, Steer, D, Tamanini, N, Tasinato, G, Torrado, J, Unal, C, Vennin, V, Vernieri, D, Vernizzi, F, Volonteri, M, Wachter, J, Wands, D, Witkowski, L, Zumalacarregui, M, Annis, J, Ares, F, Avelino, P, Avgoustidis, A, Barausse, E, Bonilla, A, Bonvin, C, Bosso, P, Calabrese, M, Caliskan, M, Cembranos, J, Chala, M, Chernoff, D, Clough, K, Criswell, A, Das, S, Silva, A, Dayal, P, Domcke, V, Durrer, R, Easther, R, Escoffier, S, Ferrans, S, Fryer, C, Gair, J, Gordon, C, Hendry, M, Hindmarsh, M, Hooper, D, Kajfasz, E, Kopp, J, Koushiappas, S, Kumar, U, Kunz, M, Lagos, M, Lilley, M, Lizarraga, J, Lobo, F, Maleknejad, A, Martins, C, Meerburg, P, Meyer, R, Mimoso, J, Nesseris, S, Nunes, N, Oikonomou, V, Orlando, G, Ozsoy, O, Pacucci, F, Palmese, A, Petiteau, A, Pinol, L, Zwart, S, Pratten, G, Prokopec, T, Quenby, J, Rastgoo, S, Roest, D, Rummukainen, K, Schimd, C, Secroun, A, Sesana, A, Sopuerta, C, Tereno, I, Tolley, A, Urrestilla, J, Vagenas, E, van de Vis, J, van de Weygaert, R, Wardell, B, Weir, D, White, G, Swiezewska, B, Zhdanov, V, Auclair P., Bacon D., Baker T., Barreiro T., Bartolo N., Belgacem E., Bellomo N., Ben-Dayan I., Bertacca D., Besancon M., Blanco-Pillado J. J., Blas D., Boileau G., Calcagni G., Caldwell R., Caprini C., Carbone C., Chang C. -F., Chen H. -Y., Christensen N., Clesse S., Comelli D., Congedo G., Contaldi C., Crisostomi M., Croon D., Cui Y., Cusin G., Cutting D., Dalang C., De Luca V., Pozzo W. D., Desjacques V., Dimastrogiovanni E., Dorsch G. C., Ezquiaga J. M., Fasiello M., Figueroa D. G., Flauger R., Franciolini G., Frusciante N., Fumagalli J., Garcia-Bellido J., Gould O., Holz D., Iacconi L., Jain R. K., Jenkins A. C., Jinno R., Joana C., Karnesis N., Konstandin T., Koyama K., Kozaczuk J., Kuroyanagi S., Laghi D., Lewicki M., Lombriser L., Madge E., Maggiore M., Malhotra A., Mancarella M., Mandic V., Mangiagli A., Matarrese S., Mazumdar A., Mukherjee S., Musco I., Nardini G., No J. M., Papanikolaou T., Peloso M., Pieroni M., Pilo L., Raccanelli A., Renaux-Petel S., Renzini A. I., Ricciardone A., Riotto A., Romano J. D., Rollo R., Pol A. R., Morales E. R., Sakellariadou M., Saltas I. D., Scalisi M., Schmitz K., Schwaller P., Sergijenko O., Servant G., Simakachorn P., Sorbo L., Sousa L., Speri L., Steer D. A., Tamanini N., Tasinato G., Torrado J., Unal C., Vennin V., Vernieri D., Vernizzi F., Volonteri M., Wachter J. M., Wands D., Witkowski L. T., Zumalacarregui M., Annis J., Ares F. R., Avelino P. P., Avgoustidis A., Barausse E., Bonilla A., Bonvin C., Bosso P., Calabrese M., Caliskan M., Cembranos J. A. R., Chala M., Chernoff D., Clough K., Criswell A., Das S., Silva A., Dayal P., Domcke V., Durrer R., Easther R., Escoffier S., Ferrans S., Fryer C., Gair J., Gordon C., Hendry M., Hindmarsh M., Hooper D. C., Kajfasz E., Kopp J., Koushiappas S. M., Kumar U., Kunz M., Lagos M., Lilley M., Lizarraga J., Lobo F. S. N., Maleknejad A., Martins C. J. A. P., Meerburg P. D., Meyer R., Mimoso J. P., Nesseris S., Nunes N., Oikonomou V., Orlando G., Ozsoy O., Pacucci F., Palmese A., Petiteau A., Pinol L., Zwart S. P., Pratten G., Prokopec T., Quenby J., Rastgoo S., Roest D., Rummukainen K., Schimd C., Secroun A., Sesana A., Sopuerta C. F., Tereno I., Tolley A., Urrestilla J., Vagenas E. C., van de Vis J., van de Weygaert R., Wardell B., Weir D. J., White G., Swiezewska B., Zhdanov V. I., Auclair, P, Bacon, D, Baker, T, Barreiro, T, Bartolo, N, Belgacem, E, Bellomo, N, Ben-Dayan, I, Bertacca, D, Besancon, M, Blanco-Pillado, J, Blas, D, Boileau, G, Calcagni, G, Caldwell, R, Caprini, C, Carbone, C, Chang, C, Chen, H, Christensen, N, Clesse, S, Comelli, D, Congedo, G, Contaldi, C, Crisostomi, M, Croon, D, Cui, Y, Cusin, G, Cutting, D, Dalang, C, De Luca, V, Pozzo, W, Desjacques, V, Dimastrogiovanni, E, Dorsch, G, Ezquiaga, J, Fasiello, M, Figueroa, D, Flauger, R, Franciolini, G, Frusciante, N, Fumagalli, J, Garcia-Bellido, J, Gould, O, Holz, D, Iacconi, L, Jain, R, Jenkins, A, Jinno, R, Joana, C, Karnesis, N, Konstandin, T, Koyama, K, Kozaczuk, J, Kuroyanagi, S, Laghi, D, Lewicki, M, Lombriser, L, Madge, E, Maggiore, M, Malhotra, A, Mancarella, M, Mandic, V, Mangiagli, A, Matarrese, S, Mazumdar, A, Mukherjee, S, Musco, I, Nardini, G, No, J, Papanikolaou, T, Peloso, M, Pieroni, M, Pilo, L, Raccanelli, A, Renaux-Petel, S, Renzini, A, Ricciardone, A, Riotto, A, Romano, J, Rollo, R, Pol, A, Morales, E, Sakellariadou, M, Saltas, I, Scalisi, M, Schmitz, K, Schwaller, P, Sergijenko, O, Servant, G, Simakachorn, P, Sorbo, L, Sousa, L, Speri, L, Steer, D, Tamanini, N, Tasinato, G, Torrado, J, Unal, C, Vennin, V, Vernieri, D, Vernizzi, F, Volonteri, M, Wachter, J, Wands, D, Witkowski, L, Zumalacarregui, M, Annis, J, Ares, F, Avelino, P, Avgoustidis, A, Barausse, E, Bonilla, A, Bonvin, C, Bosso, P, Calabrese, M, Caliskan, M, Cembranos, J, Chala, M, Chernoff, D, Clough, K, Criswell, A, Das, S, Silva, A, Dayal, P, Domcke, V, Durrer, R, Easther, R, Escoffier, S, Ferrans, S, Fryer, C, Gair, J, Gordon, C, Hendry, M, Hindmarsh, M, Hooper, D, Kajfasz, E, Kopp, J, Koushiappas, S, Kumar, U, Kunz, M, Lagos, M, Lilley, M, Lizarraga, J, Lobo, F, Maleknejad, A, Martins, C, Meerburg, P, Meyer, R, Mimoso, J, Nesseris, S, Nunes, N, Oikonomou, V, Orlando, G, Ozsoy, O, Pacucci, F, Palmese, A, Petiteau, A, Pinol, L, Zwart, S, Pratten, G, Prokopec, T, Quenby, J, Rastgoo, S, Roest, D, Rummukainen, K, Schimd, C, Secroun, A, Sesana, A, Sopuerta, C, Tereno, I, Tolley, A, Urrestilla, J, Vagenas, E, van de Vis, J, van de Weygaert, R, Wardell, B, Weir, D, White, G, Swiezewska, B, Zhdanov, V, Auclair P., Bacon D., Baker T., Barreiro T., Bartolo N., Belgacem E., Bellomo N., Ben-Dayan I., Bertacca D., Besancon M., Blanco-Pillado J. J., Blas D., Boileau G., Calcagni G., Caldwell R., Caprini C., Carbone C., Chang C. -F., Chen H. -Y., Christensen N., Clesse S., Comelli D., Congedo G., Contaldi C., Crisostomi M., Croon D., Cui Y., Cusin G., Cutting D., Dalang C., De Luca V., Pozzo W. D., Desjacques V., Dimastrogiovanni E., Dorsch G. C., Ezquiaga J. M., Fasiello M., Figueroa D. G., Flauger R., Franciolini G., Frusciante N., Fumagalli J., Garcia-Bellido J., Gould O., Holz D., Iacconi L., Jain R. K., Jenkins A. C., Jinno R., Joana C., Karnesis N., Konstandin T., Koyama K., Kozaczuk J., Kuroyanagi S., Laghi D., Lewicki M., Lombriser L., Madge E., Maggiore M., Malhotra A., Mancarella M., Mandic V., Mangiagli A., Matarrese S., Mazumdar A., Mukherjee S., Musco I., Nardini G., No J. M., Papanikolaou T., Peloso M., Pieroni M., Pilo L., Raccanelli A., Renaux-Petel S., Renzini A. I., Ricciardone A., Riotto A., Romano J. D., Rollo R., Pol A. R., Morales E. R., Sakellariadou M., Saltas I. D., Scalisi M., Schmitz K., Schwaller P., Sergijenko O., Servant G., Simakachorn P., Sorbo L., Sousa L., Speri L., Steer D. A., Tamanini N., Tasinato G., Torrado J., Unal C., Vennin V., Vernieri D., Vernizzi F., Volonteri M., Wachter J. M., Wands D., Witkowski L. T., Zumalacarregui M., Annis J., Ares F. R., Avelino P. P., Avgoustidis A., Barausse E., Bonilla A., Bonvin C., Bosso P., Calabrese M., Caliskan M., Cembranos J. A. R., Chala M., Chernoff D., Clough K., Criswell A., Das S., Silva A., Dayal P., Domcke V., Durrer R., Easther R., Escoffier S., Ferrans S., Fryer C., Gair J., Gordon C., Hendry M., Hindmarsh M., Hooper D. C., Kajfasz E., Kopp J., Koushiappas S. M., Kumar U., Kunz M., Lagos M., Lilley M., Lizarraga J., Lobo F. S. N., Maleknejad A., Martins C. J. A. P., Meerburg P. D., Meyer R., Mimoso J. P., Nesseris S., Nunes N., Oikonomou V., Orlando G., Ozsoy O., Pacucci F., Palmese A., Petiteau A., Pinol L., Zwart S. P., Pratten G., Prokopec T., Quenby J., Rastgoo S., Roest D., Rummukainen K., Schimd C., Secroun A., Sesana A., Sopuerta C. F., Tereno I., Tolley A., Urrestilla J., Vagenas E. C., van de Vis J., van de Weygaert R., Wardell B., Weir D. J., White G., Swiezewska B., and Zhdanov V. I.

Abstract

The Laser Interferometer Space Antenna (LISA) has two scientific objectives of cosmological focus: to probe the expansion rate of the universe, and to understand stochastic gravitational-wave backgrounds and their implications for early universe and particle physics, from the MeV to the Planck scale. However, the range of potential cosmological applications of gravitational-wave observations extends well beyond these two objectives. This publication presents a summary of the state of the art in LISA cosmology, theory and methods, and identifies new opportunities to use gravitational-wave observations by LISA to probe the universe.

Published
2023

15. Astrophysics with the Laser Interferometer Space Antenna

Author

Amaro-Seoane, P, Andrews, J, Arca Sedda, M, Askar, A, Baghi, Q, Balasov, R, Bartos, I, Bavera, S, Bellovary, J, Berry, C, Berti, E, Bianchi, S, Blecha, L, Blondin, S, Bogdanović, T, Boissier, S, Bonetti, M, Bonoli, S, Bortolas, E, Breivik, K, Capelo, P, Caramete, L, Cattorini, F, Charisi, M, Chaty, S, Chen, X, Chruślińska, M, Chua, A, Church, R, Colpi, M, D’Orazio, D, Danielski, C, Davies, M, Dayal, P, De Rosa, A, Derdzinski, A, Destounis, K, Dotti, M, Duţan, I, Dvorkin, I, Fabj, G, Foglizzo, T, Ford, S, Fouvry, J, Franchini, A, Fragos, T, Fryer, C, Gaspari, M, Gerosa, D, Graziani, L, Groot, P, Habouzit, M, Haggard, D, Haiman, Z, Han, W, Istrate, A, Johansson, P, Khan, F, Kimpson, T, Kokkotas, K, Kong, A, Korol, V, Kremer, K, Kupfer, T, Lamberts, A, Larson, S, Lau, M, Liu, D, Lloyd-Ronning, N, Lodato, G, Lupi, A, Ma, C, Maccarone, T, Mandel, I, Mangiagli, A, Mapelli, M, Mathis, S, Mayer, L, Mcgee, S, Mckernan, B, Miller, M, Mota, D, Mumpower, M, Nasim, S, Nelemans, G, Noble, S, Pacucci, F, Panessa, F, Paschalidis, V, Pfister, H, Porquet, D, Quenby, J, Ricarte, A, Röpke, F, Regan, J, Rosswog, S, Ruiter, A, Ruiz, M, Runnoe, J, Schneider, R, Amaro-Seoane P., Andrews J., Arca Sedda M., Askar A., Baghi Q., Balasov R., Bartos I., Bavera S. S., Bellovary J., Berry C. P. L., Berti E., Bianchi S., Blecha L., Blondin S., Bogdanović T., Boissier S., Bonetti M., Bonoli S., Bortolas E., Breivik K., Capelo P. R., Caramete L., Cattorini F., Charisi M., Chaty S., Chen X., Chruślińska M., Chua A. J. K., Church R., Colpi M., D’Orazio D., Danielski C., Davies M. B., Dayal P., De Rosa A., Derdzinski A., Destounis K., Dotti M., Duţan I., Dvorkin I., Fabj G., Foglizzo T., Ford S., Fouvry J. B., Franchini A., Fragos T., Fryer C., Gaspari M., Gerosa D., Graziani L., Groot P., Habouzit M., Haggard D., Haiman Z., Han W. B., Istrate A., Johansson P. H., Khan F. M., Kimpson T., Kokkotas K., Kong A., Korol V., Kremer K., Kupfer T., Lamberts A., Larson S., Lau M., Liu D., Lloyd-Ronning N., Lodato G., Lupi A., Ma C. P., Maccarone T., Mandel I., Mangiagli A., Mapelli M., Mathis S., Mayer L., McGee S., McKernan B., Miller M. C., Mota D. F., Mumpower M., Nasim S. S., Nelemans G., Noble S., Pacucci F., Panessa F., Paschalidis V., Pfister H., Porquet D., Quenby J., Ricarte A., Röpke F. K., Regan J., Rosswog S., Ruiter A., Ruiz M., Runnoe J., Schneider R., Amaro-Seoane, P, Andrews, J, Arca Sedda, M, Askar, A, Baghi, Q, Balasov, R, Bartos, I, Bavera, S, Bellovary, J, Berry, C, Berti, E, Bianchi, S, Blecha, L, Blondin, S, Bogdanović, T, Boissier, S, Bonetti, M, Bonoli, S, Bortolas, E, Breivik, K, Capelo, P, Caramete, L, Cattorini, F, Charisi, M, Chaty, S, Chen, X, Chruślińska, M, Chua, A, Church, R, Colpi, M, D’Orazio, D, Danielski, C, Davies, M, Dayal, P, De Rosa, A, Derdzinski, A, Destounis, K, Dotti, M, Duţan, I, Dvorkin, I, Fabj, G, Foglizzo, T, Ford, S, Fouvry, J, Franchini, A, Fragos, T, Fryer, C, Gaspari, M, Gerosa, D, Graziani, L, Groot, P, Habouzit, M, Haggard, D, Haiman, Z, Han, W, Istrate, A, Johansson, P, Khan, F, Kimpson, T, Kokkotas, K, Kong, A, Korol, V, Kremer, K, Kupfer, T, Lamberts, A, Larson, S, Lau, M, Liu, D, Lloyd-Ronning, N, Lodato, G, Lupi, A, Ma, C, Maccarone, T, Mandel, I, Mangiagli, A, Mapelli, M, Mathis, S, Mayer, L, Mcgee, S, Mckernan, B, Miller, M, Mota, D, Mumpower, M, Nasim, S, Nelemans, G, Noble, S, Pacucci, F, Panessa, F, Paschalidis, V, Pfister, H, Porquet, D, Quenby, J, Ricarte, A, Röpke, F, Regan, J, Rosswog, S, Ruiter, A, Ruiz, M, Runnoe, J, Schneider, R, Amaro-Seoane P., Andrews J., Arca Sedda M., Askar A., Baghi Q., Balasov R., Bartos I., Bavera S. S., Bellovary J., Berry C. P. L., Berti E., Bianchi S., Blecha L., Blondin S., Bogdanović T., Boissier S., Bonetti M., Bonoli S., Bortolas E., Breivik K., Capelo P. R., Caramete L., Cattorini F., Charisi M., Chaty S., Chen X., Chruślińska M., Chua A. J. K., Church R., Colpi M., D’Orazio D., Danielski C., Davies M. B., Dayal P., De Rosa A., Derdzinski A., Destounis K., Dotti M., Duţan I., Dvorkin I., Fabj G., Foglizzo T., Ford S., Fouvry J. B., Franchini A., Fragos T., Fryer C., Gaspari M., Gerosa D., Graziani L., Groot P., Habouzit M., Haggard D., Haiman Z., Han W. B., Istrate A., Johansson P. H., Khan F. M., Kimpson T., Kokkotas K., Kong A., Korol V., Kremer K., Kupfer T., Lamberts A., Larson S., Lau M., Liu D., Lloyd-Ronning N., Lodato G., Lupi A., Ma C. P., Maccarone T., Mandel I., Mangiagli A., Mapelli M., Mathis S., Mayer L., McGee S., McKernan B., Miller M. C., Mota D. F., Mumpower M., Nasim S. S., Nelemans G., Noble S., Pacucci F., Panessa F., Paschalidis V., Pfister H., Porquet D., Quenby J., Ricarte A., Röpke F. K., Regan J., Rosswog S., Ruiter A., Ruiz M., Runnoe J., and Schneider R.

Abstract

The Laser Interferometer Space Antenna (LISA) will be a transformative experiment for gravitational wave astronomy, and, as such, it will offer unique opportunities to address many key astrophysical questions in a completely novel way. The synergy with ground-based and space-born instruments in the electromagnetic domain, by enabling multi-messenger observations, will add further to the discovery potential of LISA. The next decade is crucial to prepare the astrophysical community for LISA’s first observations. This review outlines the extensive landscape of astrophysical theory, numerical simulations, and astronomical observations that are instrumental for modeling and interpreting the upcoming LISA datastream. To this aim, the current knowledge in three main source classes for LISA is reviewed; ultra-compact stellar-mass binaries, massive black hole binaries, and extreme or interme-diate mass ratio inspirals. The relevant astrophysical processes and the established modeling techniques are summarized. Likewise, open issues and gaps in our understanding of these sources are highlighted, along with an indication of how LISA could help making progress in the different areas. New research avenues that LISA itself, or its joint exploitation with upcoming studies in the electromagnetic domain, will enable, are also illustrated. Improvements in modeling and analysis approaches, such as the combination of numerical simulations and modern data science techniques, are discussed. This review is intended to be a starting point for using LISA as a new discovery tool for understanding our Universe.

Published
2023

16. JWST: Probing the Epoch of Reionization with a Wide Field Time-Domain Survey

Author

Wang, Lifan, Mould, J., Baade, D., Baron, E., Bromm, V., Cooke, J., Fan, X., Foley, R., Fruchter, A., Gal-Yam, A., Heger, A., Höflich, P., Howell, D. A., Kashlinsky, A., Koekemoer, A., Mather, J., Mazzali, P., Pacucci, F., Patat, F., Pian, E., Perlmutter, S., Rest, A., Rubin, D., Sand, D., Stubbs, C., Suntzeff, N., Wang, X. -F., Whalen, D., Wheeler, J. C., Yue, B., and Astronomy

Subjects
General Relativity and Quantum Cosmology, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

A public deep and wide science enabling survey will be needed to discover these black holes and supernovae, and to cover the area large enough for cosmic infrared background to be reliably studied. This enabling survey will find a large number of other transients and enable supernova cosmology up to z 5.

Published
2019

17. A Gravitationally Lensed Quasar at the Epoch of Reionization

Author

Fan, X., Wang, F., Yang, J., Keeton, C., Yue, M., Zabludoff, A., Bian, F., Bonaglia, M., Georgiev, I., Hennawi, J., Li, J., McGreer, I., Naidu, R., Pacucci, F., Rabien, S., Thompson, D., Venemans, B., Walter, F., Wu, X., and wang, r.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

A high fraction of the most luminous high-redshift quasars was predicted to be lensed due to magnification bias. We report the discovery of a strongly lensed ultraluminous quasar at z = 6.51, the first such object detected at the epoch of reionization and the brightest quasar yet known at z > 5. High-resolution HST imaging reveals a multiple imaged system with a maximum image separation 0.2", best explained by a model of three quasar images lensed by a low luminosity galaxy at z~0.7, with a magnification factor of ~50. This discovery suggests that a significant population of strongly lensed, high redshift quasars could have been missed by previous surveys, as standard color selection fails when the quasar color is contaminated by the lensing galaxy flux.

Published
2019

18. Glimmering in the Dark: Modeling the Low-mass End of the M ∙-σ Relation and of the Quasar Luminosity Function

Author

Pacucci, F., Loeb, A., Mezcua, M., and Martín-Navarro, I.

Abstract

The {M}\bullet {--}σ relation establishes a connection between central black holes (BHs) and their host spheroids. Supported by observations at {M}\bullet ≳ {10}5 {M}☉ , there is limited data on its validity at lower masses. Employing a semi-analytical model to simulate the combined evolution of BHs and their host galaxies, we predict the observational consequences of assuming a bimodality in the accretion efficiency of BHs, with low-mass BHs ({M}\bullet ≲ {10}5 {M}☉ ) accreting inefficiently. We predict a departure from the {M}\bullet {--}σ relation at a transitional BH mass ̃ {10}5 {M}☉ , with lower-mass BHs unable to reach the mass dictated by the relation and becoming disconnected from the evolution of the host galaxy. This prediction is an alternative to previous works suggesting a flattening of the relation at ̃ {10}5{--}{10}6 {M}☉ . Furthermore, we predict a deficit of BHs shining at bolometric luminosities ̃ {10}42 {erg} {{{s}}}-1. Joined with a detection bias, this could partly explain the scarce number of intermediate-mass BHs detected. Conversely, we predict an increase in source density at lower bolometric luminosities, < {10}42 {erg} {{{s}}}-1. Because our predictions assume a bimodal population of high-redshift BH seeds, future observations of fainter BHs will be fundamental for constraining the nature of these seeds.

Published
2018

20. The brightest Ly alpha emitter:Pop III or black hole?

Author

Pallottini, A., Ferrara, A., Pacucci, F., Gallerani, S., Salvadori, S., Schneider, R., Schaerer, D., Sobral, D., Matthee, J., Pallottini, A., Ferrara, A., Pacucci, F., Gallerani, S., Salvadori, S., Schneider, R., Schaerer, D., Sobral, D., and Matthee, J.

Abstract

CR7 is the brightest z = 6.6 Ly alpha emitter (LAE) known to date, and spectroscopic follow-up by Sobral et al. suggests that CR7 might host Population (Pop) III stars. We examine this interpretation using cosmological hydrodynamical simulations. Several simulated galaxies show the same 'Pop III wave' pattern observed in CR7. However, to reproduce the extreme CR7 Ly alpha/He II1640 line luminosities (L-alpha/He II) a top-heavy initial mass function and a massive (greater than or similar to 10(7)M(circle dot)) Pop III burst with age less than or similar to 2 Myr are required. Assuming that the observed properties of Ly alpha and He II emission are typical for Pop III, we predict that in the COSMOS/UDS/SA22 fields, 14 out of the 30 LAEs at z = 6.6 with L-alpha > 10(43.3) erg s(-1) should also host Pop III stars producing an observable L-He II greater than or similar to 10(42.7) erg s(-1). As an alternate explanation, we explore the possibility that CR7 is instead powered by accretion on to a direct collapse black hole. Our model predicts L-alpha, L-He II, and X-ray luminosities that are in agreement with the observations. In any case, the observed properties of CR7 indicate that this galaxy is most likely powered by sources formed from pristine gas. We propose that further X-ray observations can distinguish between the two above scenarios.

Published
2015

21. The brightest Ly alpha emitter : Pop III or black hole?

Author

Pallottini, A., Ferrara, A., Pacucci, F., Gallerani, S., Salvadori, S., Schneider, R., Schaerer, D., Sobral, D., Matthee, J., Pallottini, A., Ferrara, A., Pacucci, F., Gallerani, S., Salvadori, S., Schneider, R., Schaerer, D., Sobral, D., and Matthee, J.

Abstract

CR7 is the brightest z = 6.6 Ly alpha emitter (LAE) known to date, and spectroscopic follow-up by Sobral et al. suggests that CR7 might host Population (Pop) III stars. We examine this interpretation using cosmological hydrodynamical simulations. Several simulated galaxies show the same 'Pop III wave' pattern observed in CR7. However, to reproduce the extreme CR7 Ly alpha/He II1640 line luminosities (L-alpha/He II) a top-heavy initial mass function and a massive (greater than or similar to 10(7)M(circle dot)) Pop III burst with age less than or similar to 2 Myr are required. Assuming that the observed properties of Ly alpha and He II emission are typical for Pop III, we predict that in the COSMOS/UDS/SA22 fields, 14 out of the 30 LAEs at z = 6.6 with L-alpha > 10(43.3) erg s(-1) should also host Pop III stars producing an observable L-He II greater than or similar to 10(42.7) erg s(-1). As an alternate explanation, we explore the possibility that CR7 is instead powered by accretion on to a direct collapse black hole. Our model predicts L-alpha, L-He II, and X-ray luminosities that are in agreement with the observations. In any case, the observed properties of CR7 indicate that this galaxy is most likely powered by sources formed from pristine gas. We propose that further X-ray observations can distinguish between the two above scenarios.

Published
2015

22. The brightest Ly α emitter: Pop III or black hole?

Author

Pallottini, A., primary, Ferrara, A., additional, Pacucci, F., additional, Gallerani, S., additional, Salvadori, S., additional, Schneider, R., additional, Schaerer, D., additional, Sobral, D., additional, and Matthee, J., additional

Published
2015
Full Text
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23. Physical Properties of the First Quasars

Author

Gallerani, S, Fan, X, Maiolino, R, and Pacucci, F

Subjects
galaxies: high redshift, 13. Climate action, Astrophysics::High Energy Astrophysical Phenomena, quasars: supermassive black holes, Astrophysics::Cosmology and Extragalactic Astrophysics, emission lines, Astrophysics::Galaxy Astrophysics, ISM
Abstract

Since the beginning of the new millennium, more than 100 $z\sim 6$ quasars have been discovered through several surveys and followed-up with multi-wavelength observations. These data provided a large amount of information on the growth of supermassive black holes at the early epochs, the properties of quasar host galaxies and the joint formation and evolution of these massive systems. We review the properties of the highest-$z$ quasars known so far, especially focusing on some of the most recent results obtained in (sub-)millimeter bands. We discuss key observational challenges and open issues in theoretical models and highlight possible new strategies to improve our understanding of the galaxy-black hole formation and evolution in the early Universe.

25. Astrophysics with the Laser Interferometer Space Antenna

Author

Seoane, Pau Amaro, Andrews, Jeff, Sedda, Manuel Arca, Askar, Abbas, Baghi, Quentin, Balasov, Razvan, Bartos, Imre, Bavera, Simone S., Bellovary, Jillian, Berry, Christopher P. L., Berti, Emanuele, Bianchi, Stefano, Blecha, Laura, Blondin, Stephane, Bogdanović, Tamara, Boissier, Samuel, Bonetti, Matteo, Bonoli, Silvia, Bortolas, Elisa, Breivik, Katelyn, Capelo, Pedro R., Caramete, Laurentiu, Cattorini, Federico, Charisi, Maria, Chaty, Sylvain, Chen, Xian, Chruślińska, Martyna, Chua, Alvin J. K., Church, Ross, Colpi, Monica, D'Orazio, Daniel, Danielski, Camilla, Davies, Melvyn B., Dayal, Pratika, De Rosa, Alessandra, Derdzinski, Andrea, Destounis, Kyriakos, Dotti, Massimo, Duţan, Ioana, Dvorkin, Irina, Fabj, Gaia, Foglizzo, Thierry, Ford, Saavik, Fouvry, Jean-Baptiste, Franchini, Alessia, Fragos, Tassos, Fryer, Chris, Gaspari, Massimo, Gerosa, Davide, Graziani, Luca, Groot, Paul, Habouzit, Melanie, Haggard, Daryl, Haiman, Zoltan, Han, Wen-Biao, Istrate, Alina, Johansson, Peter H., Khan, Fazeel Mahmood, Kimpson, Tomas, Kokkotas, Kostas, Kong, Albert, Korol, Valeriya, Kremer, Kyle, Kupfer, Thomas, Lamberts, Astrid, Larson, Shane, Lau, Mike, Liu, Dongliang, Lloyd-Ronning, Nicole, Lodato, Giuseppe, Lupi, Alessandro, Ma, Chung-Pei, Maccarone, Tomas, Mandel, Ilya, Mangiagli, Alberto, Mapelli, Michela, Mathis, Steéphane, Mayer, Lucio, McGee, Sean, McKernan, Berry, Miller, M. Coleman, Mota, David F., Mumpower, Matthew, Nasim, Syeda S, Nelemans, Gijs, Noble, Scott, Pacucci, Fabio, Panessa, Francesca, Paschalidis, Vasileio, Pfister, Hugo, Porquet, Delphine, Quenby, John, Ricarte, Angelo, Röpke, Friedrich K., Regan, John, Rosswog, Stephan, Ruiter, Ashley, Ruiz, Milton, Runnoe, Jessie, Schneider, Raffaella, Schnittman, Jeremy, Secunda, Amy, Sesana, Alberto, Seto, Naoki, Shao, Lijing, Shapiro, Stuart, Sopuerta, Carlos, Stone, Nicholas C., Suvorov, Arthur, Tamanini, Nicola, Tamfal, Tomas, Tauris, Thomas, Temmink, Karel, Tomsick, John, Toonen, Silvia, Torres-Orjuela, Alejandro, Toscani, Martina, Tsokaros, Antonios, Unal, Caner, Vázquez-Aceves, Verónica, Valiante, Rosa, van Putten, Maurice, van Roestel, Jan, Vignali, Christian, Volonteri, Marta, Wu, Kinwah, Younsi, Ziri, Yu, Shenghua, Zane, Silvia, Zwick, Lorenz, Antonini, Fabio, Baibhav, Vishal, Barausse, Enrico, Rivera, Alexander Bonilla, Branchesi, Marica, Branduardi-Raymont, Graziella, Burdge, Kevin, Chakraborty, Srija, Cuadra, Jorge, Dage, Kristen, Davis, Benjamin, de Mink, Selma E., Decarli, Roberto, Doneva, Daniela, Escoffier, Stephanie, Fragione, Giacomo, Gandhi, Poshak, Haardt, Francesco, Lousto, Carlos O., Nissanke, Samaya, Nordhaus, Jason, O'Shaughnessy, Richard, Zwart, Simon Portegies, Pound, Adam, Schussler, Fabian, Sergijenko, Olga, Spallicci, Alessandro, Vernieri, Daniele, Vigna-Gómez, Alejandro, Amaro-Seoane, Pau, Andrews, Jeff, Arca Sedda, Manuel, Askar, Abba, Baghi, Quentin, Balasov, Razvan, Bartos, Imre, Bavera, Simone S., Bellovary, Jillian, Berry, Christopher P. L., Berti, Emanuele, Bianchi, Stefano, Blecha, Laura, Blondin, Stéphane, Bogdanović, Tamara, Boissier, Samuel, Bonetti, Matteo, Bonoli, Silvia, Bortolas, Elisa, Breivik, Katelyn, Capelo, Pedro R., Caramete, Laurentiu, Cattorini, Federico, Charisi, Maria, Chaty, Sylvain, Chen, Xian, Chruślińska, Martyna, Chua, Alvin J. K., Church, Ro, Colpi, Monica, D’Orazio, Daniel, Danielski, Camilla, Davies, Melvyn B., Dayal, Pratika, De Rosa, Alessandra, Derdzinski, Andrea, Destounis, Kyriako, Dotti, Massimo, Duţan, Ioana, Dvorkin, Irina, Fabj, Gaia, Foglizzo, Thierry, Ford, Saavik, Fouvry, Jean-Baptiste, Franchini, Alessia, Fragos, Tasso, Fryer, Chri, Gaspari, Massimo, Gerosa, Davide, Graziani, Luca, Groot, Paul, Habouzit, Melanie, Haggard, Daryl, Haiman, Zoltan, Han, Wen-Biao, Istrate, Alina, Johansson, Peter H., Khan, Fazeel Mahmood, Kimpson, Toma, Kokkotas, Kosta, Kong, Albert, Korol, Valeriya, Kremer, Kyle, Kupfer, Thoma, Lamberts, Astrid, Larson, Shane, Lau, Mike, Liu, Dongliang, Lloyd-Ronning, Nicole, Lodato, Giuseppe, Lupi, Alessandro, Ma, Chung-Pei, Maccarone, Toma, Mandel, Ilya, Mangiagli, Alberto, Mapelli, Michela, Mathis, Stéphane, Mayer, Lucio, Mcgee, Sean, Mckernan, Berry, Miller, M. Coleman, Mota, David F., Mumpower, Matthew, Nasim, Syeda S., Nelemans, Gij, Noble, Scott, Pacucci, Fabio, Panessa, Francesca, Paschalidis, Vasileio, Pfister, Hugo, Porquet, Delphine, Quenby, John, Ricarte, Angelo, Röpke, Friedrich K., Regan, John, Rosswog, Stephan, Ruiter, Ashley, Ruiz, Milton, Runnoe, Jessie, Schneider, Raffaella, Schnittman, Jeremy, Secunda, Amy, Sesana, Alberto, Seto, Naoki, Shao, Lijing, Shapiro, Stuart, Sopuerta, Carlo, Stone, Nicholas C., Suvorov, Arthur, Tamanini, Nicola, Tamfal, Toma, Tauris, Thoma, Temmink, Karel, Tomsick, John, Toonen, Silvia, Torres-Orjuela, Alejandro, Toscani, Martina, Tsokaros, Antonio, Unal, Caner, Vázquez-Aceves, Verónica, Valiante, Rosa, van Putten, Maurice, van Roestel, Jan, Vignali, Christian, Volonteri, Marta, Wu, Kinwah, Younsi, Ziri, Yu, Shenghua, Zane, Silvia, Zwick, Lorenz, Antonini, Fabio, Baibhav, Vishal, Barausse, Enrico, Bonilla Rivera, Alexander, Branchesi, Marica, Branduardi-Raymont, Graziella, Burdge, Kevin, Chakraborty, Srija, Cuadra, Jorge, Dage, Kristen, Davis, Benjamin, de Mink, Selma E., Decarli, Roberto, Doneva, Daniela, Escoffier, Stephanie, Gandhi, Poshak, Haardt, Francesco, Lousto, Carlos O., Nissanke, Samaya, Nordhaus, Jason, O’Shaughnessy, Richard, Portegies Zwart, Simon, Pound, Adam, Schussler, Fabian, Sergijenko, Olga, Spallicci, Alessandro, Vernieri, Daniele, Vigna-Gómez, Alejandro, Max Planck Institute for Gravitational Physics (Albert Einstein Institute) (AEI), Max-Planck-Gesellschaft, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics, Columbia University, Columbia University [New York], Department of Physics and Astronomy [Nashville], Vanderbilt University [Nashville], Fisk University, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des deux Infinis de Toulouse (L2IT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Amaro-Seoane, P, Andrews, J, Arca Sedda, M, Askar, A, Baghi, Q, Balasov, R, Bartos, I, Bavera, S, Bellovary, J, Berry, C, Berti, E, Bianchi, S, Blecha, L, Blondin, S, Bogdanović, T, Boissier, S, Bonetti, M, Bonoli, S, Bortolas, E, Breivik, K, Capelo, P, Caramete, L, Cattorini, F, Charisi, M, Chaty, S, Chen, X, Chruślińska, M, Chua, A, Church, R, Colpi, M, D’Orazio, D, Danielski, C, Davies, M, Dayal, P, De Rosa, A, Derdzinski, A, Destounis, K, Dotti, M, Duţan, I, Dvorkin, I, Fabj, G, Foglizzo, T, Ford, S, Fouvry, J, Franchini, A, Fragos, T, Fryer, C, Gaspari, M, Gerosa, D, Graziani, L, Groot, P, Habouzit, M, Haggard, D, Haiman, Z, Han, W, Istrate, A, Johansson, P, Khan, F, Kimpson, T, Kokkotas, K, Kong, A, Korol, V, Kremer, K, Kupfer, T, Lamberts, A, Larson, S, Lau, M, Liu, D, Lloyd-Ronning, N, Lodato, G, Lupi, A, Ma, C, Maccarone, T, Mandel, I, Mangiagli, A, Mapelli, M, Mathis, S, Mayer, L, Mcgee, S, Mckernan, B, Miller, M, Mota, D, Mumpower, M, Nasim, S, Nelemans, G, Noble, S, Pacucci, F, Panessa, F, Paschalidis, V, Pfister, H, Porquet, D, Quenby, J, Ricarte, A, Röpke, F, Regan, J, Rosswog, S, Ruiter, A, Ruiz, M, Runnoe, J, Schneider, R, Ministerio de Ciencia e Innovación (España), European Research Council, European Commission, Istituto Nazionale di Astrofisica, Agenzia Spaziale Italiana, and National Aeronautics and Space Administration (US)

Subjects
Astrofísica, ACTIVE GALACTIC NUCLEI, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), Black hole, Astronomy, Stellar remnant, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), TIDAL DISRUPTION EVENTS, General Relativity and Quantum Cosmology, Gravitational waves, MOCCA-SURVEY DATABASE, Settore FIS/05 - Astronomia e Astrofisica, Stellar remnants, Software Science, Multi-messenger, GRAVITATIONAL-WAVE SOURCES, Instrumentation and Methods for Astrophysics (astro-ph.IM), Extreme mass ratio in-spirals, Solar and Stellar Astrophysics (astro-ph.SR), High Energy Astrophysical Phenomena (astro-ph.HE), Black holes, Data Science, Astrophysics::Instrumentation and Methods for Astrophysics, Extreme mass ratio in-spiral, AM-CVN STARS, Astrophysics - Astrophysics of Galaxies, WHITE-DWARF BINARIES, DOUBLE NEUTRON-STARS, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Astronomia, MASSIVE BLACK-HOLE, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, X-RAY BINARIES, COMMON-ENVELOPE EVOLUTION, Gravitational wave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Full list of authors: Amaro-Seoane, Pau; Andrews, Jeff; Sedda, Manuel Arca; Askar, Abbas.; Baghi, Quentin; Balasov, Razvan; Bartos, Imre; Bavera, Simone S.; Bellovary, Jillian; Berry, Christopher P. L.; Berti, Emanuele; Bianchi, Stefano; Blecha, Laura; Blondin, Stephane; Bogdanovic, Tamara; Boissier, Samuel; Bonetti, Matteo; Bonoli, Silvia; Bortolas, Elisa; Breivik, Katelyn; Capelo, Pedro R.; Caramete, Laurentiu; Cattorini, Federico; Charisi, Maria; Chaty, Sylvain; Chen, Xian; Chruslinska, Martyna; Chua, Alvin J. K.; Church, Ross; Colpi, Monica; D'Orazio, Daniel; Danielski, Camilla; Davies, Melvyn B.; Dayal, Pratika; De Rosa, Alessandra; Derdzinski, Andrea; Destounis, Kyriakos; Dotti, Massimo; Dutan, Ioana; Dvorkin, Irina; Fabj, Gaia; Foglizzo, Thierry; Ford, Saavik; Fouvry, Jean-Baptiste; Franchini, Alessia; Fragos, Tassos; Fryer, Chris; Gaspari, Massimo; Gerosa, Davide; Graziani, Luca; Groot, Paul; Habouzit, Melanie; Haggard, Daryl; Haiman, Zoltan; Han, Wen-Biao; Istrate, Alina; Johansson, Peter H.; Khan, Fazeel Mahmood; Kimpson, Tomas; Kokkotas, Kostas; Kong, Albert; Korol, Valeriya; Kremer, Kyle; Kupfer, Thomas; Lamberts, Astrid; Larson, Shane; Lau, Mike; Liu, Dongliang; Lloyd-Ronning, Nicole; Lodato, Giuseppe; Lupi, Alessandro; Ma, Chung-Pei; Maccarone, Tomas; Mandel, Ilya; Mangiagli, Alberto; Mapelli, Michela; Mathis, Stephane; Mayer, Lucio; McGee, Sean; McKernan, Berry; Miller, M. Coleman; Mota, David F.; Mumpower, Matthew; Nasim, Syeda S.; Nelemans, Gijs; Noble, Scott; Pacucci, Fabio; Panessa, Francesca; Paschalidis, Vasileios; Pfister, Hugo; Porquet, Delphine; Quenby, John; Ricarte, Angelo; Roepke, Friedrich K.; Regan, John; Rosswog, Stephan; Ruiter, Ashley; Ruiz, Milton; Runnoe, Jessie; Schneider, Raffaella; Schnittman, Jeremy; Secunda, Amy; Sesana, Alberto; Seto, Naoki; Shao, Lijing; Shapiro, Stuart; Sopuerta, Carlos; Stone, Nicholas C.; Suvorov, Arthur; Tamanini, Nicola; Tamfal, Tomas; Tauris, Thomas; Temmink, Karel; Tomsick, John; Toonen, Silvia; Torres-Orjuela, Alejandro; Toscani, Martina; Tsokaros, Antonios; Unal, Caner; Vazquez-Aceves, Veronica; Valiante, Rosa; van Putten, Maurice; van Roestel, Jan; Vignali, Christian; Volonteri, Marta; Wu, Kinwah; Younsi, Ziri; Yu, Shenghua; Zane, Silvia; Zwick, Lorenz; Antonini, Fabio; Baibhav, Vishal; Barausse, Enrico; Bonilla Rivera, Alexander; Branchesi, Marica; Branduardi-Raymont, Graziella; Burdge, Kevin; Chakraborty, Srija; Cuadra, Jorge; Dage, Kristen; Davis, Benjamin; de Mink, Selma E.; Decarli, Roberto; Doneva, Daniela; Escoffier, Stephanie; Gandhi, Poshak; Haardt, Francesco; Lousto, Carlos O.; Nissanke, Samaya; Nordhaus, Jason; O'Shaughnessy, Richard; Portegies Zwart, Simon; Pound, Adam; Schussler, Fabian; Sergijenko, Olga; Spallicci, Alessandro; Vernieri, Daniele; Vigna-Gomez, Alejandro.-- This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article's Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article's Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/., The Laser Interferometer Space Antenna (LISA) will be a transformative experiment for gravitational wave astronomy, and, as such, it will offer unique opportunities to address many key astrophysical questions in a completely novel way. The synergy with ground-based and space-born instruments in the electromagnetic domain, by enabling multi-messenger observations, will add further to the discovery potential of LISA. The next decade is crucial to prepare the astrophysical community for LISA’s first observations. This review outlines the extensive landscape of astrophysical theory, numerical simulations, and astronomical observations that are instrumental for modeling and interpreting the upcoming LISA datastream. To this aim, the current knowledge in three main source classes for LISA is reviewed; ultra-compact stellar-mass binaries, massive black hole binaries, and extreme or interme-diate mass ratio inspirals. The relevant astrophysical processes and the established modeling techniques are summarized. Likewise, open issues and gaps in our understanding of these sources are highlighted, along with an indication of how LISA could help making progress in the different areas. New research avenues that LISA itself, or its joint exploitation with upcoming studies in the electromagnetic domain, will enable, are also illustrated. Improvements in modeling and analysis approaches, such as the combination of numerical simulations and modern data science techniques, are discussed. This review is intended to be a starting point for using LISA as a new discovery tool for understanding our Universe. © The Author(s) 2023, corrected publication 2023., P. Dayal acknowledges support from the European Research council (ERC-717001) and from the Netherlands Research Council NWO (016.VIDI.189.162). P.H. Johansson acknowledges the support from the European Research Council (ERC-818930). S. Toonen acknowledges support from the Netherlands Research Council NWO (VENI 639.041.645 Grants) C. Unal is supported by European Structural and Investment Funds and the Czech Ministry of Education, Youth and Sports (Project CoGraDS - CZ.02.1.01/0.0/0.0/15_003/0000437). S. Chaty acknowledges the LabEx UnivEarthS for the funding of Interface project I10 “From binary evolution towards merging of compact objects”. A. De Rosa acknowledges financial contribution from the agreement ASI-INAF n.2017-14-H.O E. Berti is supported by NSF Grants No. PHY-1912550 and AST-2006538, NASA ATP Grants No. 17-ATP17-0225 and 19-ATP19-0051, NSF-XSEDE Grant No. PHY-090003, and NSF Grant PHY-20043. D. Gerosa is supported by European Union’s H2020 ERC Starting Grant No. 945155–GWmining, Leverhulme Trust Grant No. RPG-2019-350 and Royal Society Grant No. RGS-R2-202004. T. Bogdanovic acknowledges support by the NASA award No. 80NSSC19K0319 and by the NSF award AST-1908042. D. Porquet acknowledges funding support from CNES. C. Danielski acknowledges financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709) B.L. Davis acknowledges support from Tamkeen under the NYU Abu Dhabi Research Institute Grant CAP3. F. Pacucci acknowledges support from a Clay Fellowship by the SAO and from the Black Hole Initiative, which is funded by grants from the John Templeton Foundation and the Gordon and Betty Moore Foundation. A.J. Ruiter acknowledges support from the Australian Research Council Future Fellowship Grant FT170100243. V. Paschalidis is supported by NSF Grant PHY-1912619 and NASA Grant 80NSSC20K1542 to the University of Arizona, and NSF-XSEDE Grant TG-PHY190020. D. Haggard acknowledges support from the NSERC Discovery Grant and Canada Research Chairs programs, and the Bob Wares Science Innovation Prospectors Fund. M. Toscani acknowledges European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie Grant Agreement No. 823823 (RISE DUSTBUSTERS project) and COST Action CA16104 - Gravitational waves, black holes and fundamental physics, supported by COST (European Cooperation in Science and Technology). M. Chruslinska, A. Istrate and G. Nelemans acknowledge support from Netherlands Research Council NWO. T. Fragos and S. Bavera acknowledge support from a Swiss National Science Foundation Professorship Grant (project numbers PP00P2_176868 and PP00P2_211006)., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).

Published
2023
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26. BASS. XXI. The Data Release 2 Overview

Author

Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Franz E. Bauer, Ezequiel Treister, Richard Mushotzky, C. Megan Urry, Tonima T. Ananna, Mislav Baloković, Jakob S. den Brok, S. Bradley Cenko, Fiona Harrison, Kohei Ichikawa, Isabella Lamperti, Amy Lein, Julian E. Mejía-Restrepo, Kyuseok Oh, Fabio Pacucci, Ryan W. Pfeifle, Meredith C. Powell, George C. Privon, Federica Ricci, Mara Salvato, Kevin Schawinski, Taro Shimizu, Krista L. Smith, Daniel Stern, Koss, Mj, Trakhtenbrot, B, Ricci, C, Bauer, Fe, Treister, E, Mushotzky, R, Urry, Cm, Ananna, Tt, Balokovic, M, den Brok, J, Cenko, Sb, Harrison, F, Ichikawa, K, Lamperti, I, Lein, A, Mejia-Restrepo, Je, Oh, K, Pacucci, F, Pfeifle, Rw, Powell, Mc, Privon, Gc, Ricci, F, Salvato, M, Schawinski, K, Shimizu, T, Smith, Kl, and Stern, D

Subjects
Space and Planetary Science, Astronomy and Astrophysics
Abstract

The BAT AGN Spectroscopic Survey (BASS) is designed to provide a highly complete census of the key physical parameters of the supermassive black holes (SMBHs) that power local active galactic nuclei (AGNs) (z less than or similar to 0.3), including their bolometric luminosity (L (bol)), black hole (BH) mass (M (BH)), accretion rates (L (bol)/L (Edd)), line-of-sight gas obscuration (N (H)), and the distinctive properties of their host galaxies (e.g., star formation rates, masses, and gas fractions). We present an overview of the second data release of BASS (DR2), an unprecedented spectroscopic AGN survey in spectral range, resolution, and sensitivity, including 1449 optical (similar to 3200 angstrom-1 mu m) and 233 near-IR (1-2.5 mu m) spectra for the brightest 858 ultrahard X-ray (14-195 keV) selected AGNs across the entire sky and essentially all levels of obscuration. This release provides a highly complete set of key measurements (emission-line measurements and central velocity dispersions), with 99.9% measured redshifts and 98% BH masses estimated (for unbeamed AGNs outside the Galactic plane). The BASS DR2 AGN sample represents a unique census of nearby powerful AGNs, spanning over 5 orders of magnitude in AGN bolometric luminosity (L (bol) similar to 10(40)-10(47) erg s(-1)), BH mass (M (BH) similar to 10(5)-10(10) M (circle dot)), Eddington ratio (L (bol)/L (Edd) greater than or similar to 10(-5)), and obscuration (N (H) similar to 10(20)-10(25) cm(-2)). The public BASS DR2 sample and measurements can thus be used to answer fundamental questions about SMBH growth and its links to host galaxy evolution and feedback in the local universe, as well as open questions concerning SMBH physics. Here we provide a brief overview of the survey strategy, the key BASS DR2 measurements, data sets and catalogs, and scientific highlights from a series of DR2-based works pursued by the BASS team., The Astrophysical Journal. Supplement Series, 261, ISSN:1538-4365, ISSN:0067-0049

Published
2022

27. Unveiling the gravitational universe at μ-Hz frequencies

Author

Alberto Mangiagli, Oliver Jennrich, Lijing Shao, N. Korsakova, Simon Barke, Miguel Zumalacarregui, Alberto Sesana, Astrid Lamberts, John A. Regan, Fazeel Mahmood Khan, Kaze Wong, Peter H. Johansson, Enrico Barausse, Juan Garcia-Bellido, Matteo Bonetti, Vishal Baibhav, Surjeet Rajendran, Manuel Arca Sedda, Lucio Mayer, Marta Volonteri, Germano Nardini, Alessandro Lupi, Karan Jani, Nicola Tamanini, Zoltan Haiman, Alessandro D. A. M. Spallicci, Emanuele Berti, Niels Warburton, Chiara Caprini, Alvise Raccanelli, Fabio Pacucci, Antoine Petiteau, Valeriya Korol, Pedro R. Capelo, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire des deux Infinis de Toulouse (L2IT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Sesana, A, Korsakova, N, Sedda, M, Baibhav, V, Barausse, E, Barke, S, Berti, E, Bonetti, M, Capelo, P, Caprini, C, Garcia-Bellido, J, Haiman, Z, Jani, K, Jennrich, O, Johansson, P, Khan, F, Korol, V, Lamberts, A, Lupi, A, Mangiagli, A, Mayer, L, Nardini, G, Pacucci, F, Petiteau, A, Raccanelli, A, Rajendran, S, Regan, J, Shao, L, Spallicci, A, Tamanini, N, Volonteri, M, Warburton, N, Wong, K, Zumalacarregui, M, Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Leibniz Universität Hannover [Hannover] (LUH), Department of Physics and Astronomy [U Mississippi], The University of Mississippi [Oxford], Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne (ESA), European Space Agency (ESA), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Interactions Sol Plante Atmosphère (ISPA), Institut National de la Recherche Agronomique (INRA)-Ecole Nationale Supérieure des Sciences Agronomiques de Bordeaux-Aquitaine (Bordeaux Sciences Agro), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), University of Helsinki, Department of Physics, Doctoral Programme in Particle Physics and Universe Sciences, Particle Physics and Astrophysics, Division of Geophysics and Astronomy (-2017), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Interactions Sol Plante Atmosphère (UMR ISPA), Ecole Nationale Supérieure des Sciences Agronomiques de Bordeaux-Aquitaine (Bordeaux Sciences Agro)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), Leibniz Universität Hannover=Leibniz University Hannover, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
astronomi, Cosmology and cosmography, Milky Way science, 01 natural sciences, Cosmology, General Relativity and Quantum Cosmology, Observatory, Matematikk og Naturvitenskap: 400::Fysikk: 430::Astrofysikk, astronomi: 438 [VDP], Micro-Hz band, 010303 astronomy & astrophysics, media_common, astro-ph.HE, Physics, [PHYS]Physics [physics], General relativity and beyond, General Relativity and Cosmology, Astrophysics::Instrumentation and Methods for Astrophysics, Massive black hole binaries, Interferometry, WHITE-DWARF BINARIES, GAS, GROWTH, MASSIVE BLACK-HOLE, MILKY-WAY, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Multimessenger and multiband Astronomy, Astrophysics and Astronomy, GALACTIC NUCLEI, gr-qc, media_common.quotation_subject, Astrophysics::Cosmology and Extragalactic Astrophysics, 114 Physical sciences, Settore FIS/05 - Astronomia e Astrofisica, Pulsar, 0103 physical sciences, POST-NEWTONIAN EVOLUTION, LISA, 010308 nuclear & particles physics, Gravitational wave, Astronomy, Astronomy and Astrophysics, 115 Astronomy, Space science, Space gravitational wave detector, Universe, Galaxy, Black hole, Space and Planetary Science, [SDU]Sciences of the Universe [physics], PHASE-TRANSITION, astrofysikk, Massive black hole binarie, astro-ph.IM, HUBBLE CONSTANT
Abstract

We propose a space-based interferometer surveying the gravitational wave (GW) sky in the milli-Hz to $\mu$-Hz frequency range. By the 2040s', the $\mu$-Hz frequency band, bracketed in between the Laser Interferometer Space Antenna (LISA) and pulsar timing arrays, will constitute the largest gap in the coverage of the astrophysically relevant GW spectrum. Yet many outstanding questions related to astrophysics and cosmology are best answered by GW observations in this band. We show that a $\mu$-Hz GW detector will be a truly overarching observatory for the scientific community at large, greatly extending the potential of LISA. Conceived to detect massive black hole binaries from their early inspiral with high signal-to-noise ratio, and low-frequency stellar binaries in the Galaxy, this instrument will be a cornerstone for multimessenger astronomy from the solar neighbourhood to the high-redshift Universe., Comment: 28 pages, 8 figures; White Paper submitted to ESA's Voyage 2050 call for papers on behalf of the LISA Consortium 2050 Task Force

Published
2021
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28. BASS. XXII. The BASS DR2 AGN Catalog and Data

Author

Michael J. Koss, Claudio Ricci, Benny Trakhtenbrot, Kyuseok Oh, Jakob S. den Brok, Julian E. Mejía-Restrepo, Daniel Stern, George C. Privon, Ezequiel Treister, Meredith C. Powell, Richard Mushotzky, Franz E. Bauer, Tonima T. Ananna, Mislav Baloković, Rudolf E. Bär, George Becker, Patricia Bessiere, Leonard Burtscher, Turgay Caglar, Enrico Congiu, Phil Evans, Fiona Harrison, Marianne Heida, Kohei Ichikawa, Nikita Kamraj, Isabella Lamperti, Fabio Pacucci, Federica Ricci, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, Matthew J. Temple, C. Megan Urry, Sylvain Veilleux, Jonathan Williams, Koss, Mj, Ricci, C, Trakhtenbrot, B, Oh, K, den Brok, J, Mejia-Restrepo, Je, Stern, D, Privon, Gc, Treister, E, Powell, Mc, Mushotzky, R, Bauer, Fe, Ananna, Tt, Balokovic, M, Bar, Re, Becker, G, Bessiere, P, Burtscher, L, Caglar, T, Congiu, E, Evans, P, Harrison, F, Heida, M, Ichikawa, K, Kamraj, N, Lamperti, I, Pacucci, F, Ricci, F, Riffel, R, Rojas, Af, Schawinski, K, Temple, Mj, Urry, Cm, Veilleux, S, and Williams, J

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Active galactic nuclei, Seyfert galaxies, X-ray active galactic nuclei, Astrophysics - astrophysics of galaxies, FOS: Physical sciences, Astronomy and Astrophysics, Surveys, Sky surveys, Astrophysics - high energy astrophysical phenomena, Galaxy spectroscopy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), X-ray quasars, X-ray surveys
Abstract

We present the active galactic nucleus (AGN) catalog and optical spectroscopy for the second data release of the Swift BAT AGN Spectroscopic Survey (BASS DR2). With this DR2 release we provide 1449 optical spectra, of which 1182 are released for the first time, for the 858 hard-X-ray-selected AGNs in the Swift BAT 70-month sample. The majority of the spectra (801/1449, 55%) are newly obtained from Very Large Telescope (VLT)/X-shooter or Palomar/Doublespec. Many of the spectra have both higher resolution (R > 2500, N similar to 450) and/or very wide wavelength coverage (3200-10000 angstrom, N similar to 600) that are important for a variety of AGN and host galaxy studies. We include newly revised AGN counterparts for the full sample and review important issues for population studies, with 47 AGN redshifts determined for the first time and 790 black hole mass and accretion rate estimates. This release is spectroscopically complete for all AGNs (100%, 858/858), with 99.8% having redshift measurements (857/858) and 96% completion in black hole mass estimates of unbeamed AGNs (722/752). This AGN sample represents a unique census of the brightest hard-X-ray-selected AGNs in the sky, spanning many orders of magnitude in Eddington ratio (L/L (Edd) = 10(-5)-100), black hole mass (M (BH) = 10(5)-10(10) M (circle dot)), and AGN bolometric luminosity (L (bol) = 10(40)-10(47) erg s(-1) )., The Astrophysical Journal. Supplement Series, 261, ISSN:1538-4365, ISSN:0067-0049

Published
2022
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29. Titans of the early Universe: The Prato statement on the origin of the first supermassive black holes

Author

Andrea Ferrara, Ke-Jung Chen, Tyrone E. Woods, Fabio Pacucci, Yuexing Li, Takamitsu Tanaka, Simon C. O. Glover, Zoltan Haiman, Daniel J. Whalen, Chiaki Kobayashi, Bhaskar Agarwal, Sunmyon Chon, Muhammad Latif, Volker Bromm, Filippos Koliopanos, Alexander Heger, Mar Mezcua, Stefania Salvadori, Takashi Hosokawa, John A. Regan, Yuya Sakurai, Priyamvada Natarajan, Ralf S. Klessen, Naoki Yoshida, Martin J. Rees, Lionel Haemmerlé, Tilman Hartwig, Kohei Inayoshi, Andrew Bunker, Raffaella Schneider, Shingo Hirano, Marco Surace, Lucio Mayer, Woods, T. E., Agarwal, B., Bromm, V., Bunker, A., Chen, K. -J., Chon, S., Ferrara, A., Glover, S. C. O., Haemmerle, L., Haiman, Z., Hartwig, T., Heger, A., Hirano, S., Hosokawa, T., Inayoshi, K., Klessen, R. S., Kobayashi, C., Koliopanos, F., Latif, M. A., Li, Yuexing, Mayer, L., Mezcua, M., Natarajan, P., Pacucci, F., Rees, M. J., Regan, J. A., Sakurai, Y., Salvadori, S., Schneider, R., Surace, M., Tanaka, T. L., Whalen, D. J., Yoshida, Naoki, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
media_common.quotation_subject, first stars, first stars – quasars: supermassive black holes, FOS: Physical sciences, 01 natural sciences, massive, 0103 physical sciences, Population III, massive, binaries, supermassive black holes, high-redshift [quasars], 010303 astronomy & astrophysics, STFC, Solar and Stellar Astrophysics (astro-ph.SR), media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Supermassive black hole, 010308 nuclear & particles physics, RCUK, Astronomy, Astronomy and Astrophysics, Quasar, high-redshift – Population III, supermassive black hole [first stars - quasars], Astrophysics - Astrophysics of Galaxies, Universe, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), binarie, ST/M000958/1, high-redshift - Population III, ST/P000509/1, Astrophysics - High Energy Astrophysical Phenomena, binaries, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

In recent years, the discovery of massive quasars at z~7 has provided a striking challenge to our understanding of the origin and growth of supermassive black holes in the early Universe. Mounting observational and theoretical evidence indicates the viability of massive seeds, formed by the collapse of supermassive stars, as a progenitor model for such early, massive accreting black holes. Although considerable progress has been made in our theoretical understanding, many questions remain regarding how (and how often) such objects may form, how they live and die, and how next generation observatories may yield new insight into the origin of these primordial titans. This review focusses on our present understanding of this remarkable formation scenario, based on discussions held at the Monash Prato Centre from November 20--24, 2017, during the workshop "Titans of the Early Universe: The Origin of the First Supermassive Black Holes.", Comment: Solicited review article (accepted) for Publications of the Astronomical Society of Australia. 38 pages, 15 figures, 1 table

Published
2019
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30. Focusing on Warm Dark Matter with Lensed High-redshift Galaxies

Author

Andrei Mesinger, Zoltan Haiman, Fabio Pacucci, Pacucci, F, Mesinger, ANDREI ALBERT, and Haiman, Z.

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cold dark matter, 010308 nuclear & particles physics, Hot dark matter, Dark matter, Halo mass function, FOS: Physical sciences, Astronomy, Velocity dispersion, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Redshift, Space and Planetary Science, 0103 physical sciences, Warm dark matter, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We propose a novel use of high-redshift galaxies, discovered in deep Hubble Space Telescope (HST) fields around strong lensing clusters. These fields probe small comoving volumes (about 1000 cubic Mpc) at high magnification (�� > 10), and can detect otherwise inaccessible ultra-faint galaxies. Even a few galaxies found in such small volumes require a very high number density of collapsed dark matter (DM) halos. This implies significant primordial power on small scales, allowing these observations to rule out popular alternatives to standard cold dark matter (CDM) models, such as warm dark matter (WDM). In this work, we analytically compute WDM halo mass functions at z = 10, including the effects of both particle free-streaming and residual velocity dispersion. The preliminary number density corresponding to the two galaxies at z about 10 already detected by the Cluster Lensing And Supernova survey with Hubble (CLASH) constrains the WDM particle mass to m_x > 1 (0.9) keV at 84% (99.9%) confidence limit (for a thermal relic relativistic at decoupling). This limit depends only on the WDM halo mass function and, unlike previous constraints on m_x, is independent of any astrophysical modeling. The forthcoming HST Frontier Fields can significantly tighten these constraints., 5 pages, 3 figures - Accepted for publication on MNRAS Letters

Published
2013

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