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85 results on '"LUMINOSITY FUNCTIONS"'

1. Optical emission-line luminosity function models for populations of supernova remnants.

Author

Kopsacheili, M, Zezas, A, and Leonidaki, I

Subjects
*LUMINOSITY, *AGE distribution, *SUPERNOVA remnants, *STELLAR luminosity function, *EMISSIVITY
Abstract

We present a basic model for the calculation of the luminosity distribution of supernova remnant populations. We construct theoretical H |$\rm \alpha \,$| and joint [S  ii ]-H |$\rm \alpha \,$| luminosity functions for supernova remnants by combining prescriptions from a basic evolution model that provides the shock velocity and radius for SNRs of different age and pre-shock density, with shock excitation models that give the gas emissivity for shocks of different physical parameters. We assume a flat age distribution, and we explore the effect of different pre-shock density distributions or different magnetic parameters. We find a very good agreement between the shape of the model H |$\rm \alpha \,$| and the joint [S  ii ]-H |$\rm \alpha \,$| luminosity functions and those measured from SNR surveys in nearby galaxies. [ABSTRACT FROM AUTHOR]

Published
2022
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2. Exploring galaxy evolution with luminosity functions across cosmic time

Author

Elbert, Holly, Verma, Aprajita, Bunker, Andrew, and Jarvis, Matt

Subjects
523.1, Astrophysics, High redshift, Galaxy evolution, Luminosity functions
Abstract

In this thesis I investigate galaxy evolution by measuring the luminosity functions of galaxies across a wide range in redshift. I measure the abundances of high redshift galaxies in deep HST imaging of the GOODS-North field from the CANDELS survey. I follow this evolution to lower redshift by measuring the luminosity functions of galaxies in ground-based imaging of the XMM-LSS field from the VIDEO survey with optical data from the CFHTLS. First, at high-redshift, I identify 22 candidate z ≈ 7 and 6 candidate z ≈ 8 − 9 galaxies. By comparing the number of candidate galaxies with those found in the GOODS-South field, I determine that cosmic variance is not the dominant source of uncertainty on the number counts. I constrain the Schechter parameters for the UV luminosity function at z ≈ 7 and z ≈ 8 − 9, finding evidence for evolution in the number density of high redshift galaxies. Next, I present the Ks-band luminosity functions in the 1 degree2 and 4.5 degree2 overlaps between the VIDEO-XMM field and the CFHTLS-D1 and CFHTLS-W1 fields. I measure the luminosity functions with the 1/Vmax method over the range 0.2 < z < 3 in VIDEO-CFHTLS-D1, and over the range 0.2 < z < 1.5 in the shallower VIDEO-CFHTLS-W1 field. I find the evolution of these luminosity functions is best described by luminosity dependent density evolution, where the characteristic magnitude has dimmed at a constant rate since z = 3, while the density has increased since z = 3, first rapidly from z = 3 to z ≈ 1.5 and then more slowly from z ≈ 1.5 to z = 0.2. I measure a significant upturn at the faint end of the luminosity function at low redshift. Finally, I compare the VIDEO-CFHTLS-D1 and VIDEO-CFHTLS-W1 luminosity functions with predicted K-band luminosity functions from the Horizon-AGN simulation. I find both an over-prediction in the numbers of faint galaxies and an under-prediction in the numbers of bright galaxies, implying that the feedback from supernovae is insufficient while the feedback from AGN is over-sufficient.

Published
2016

3. White dwarf luminosity functions from the Pan-STARRS1 3π survey

Author

Lam, Marco Cheuk-Yin, Hambly, Nigel, and Ferguson, Annette

Subjects
523.8, white dwarf, interstellar reddening, luminosity functions, motion
Abstract

White dwarfs are among the most common objects in the stellar halo; however, due to their low luminosity and low number density compared to the stars in the discs of the Milky Way, they are scarce in the observable volume. Hence, they are still poorly understood one hundred years after their discovery as relatively few have been observed. They are crucial to the understanding of several fundamental properties of the Galaxy – the geometry, kinematics and star formation history, as well as to the study of the end-stage of stellar evolution for low- and intermediate-mass stars. White dwarfs were traditionally identified by their ultraviolet (UV) excess, however, if they have cooled for a long time, they become so faint in that part of the spectrum that they cannot be seen by the most sensitive modern detectors. Proper motion was then used as a means to identify white dwarf candidates, due to their relatively large space motions compared to other objects with the same colour. The use of proper motion as a selection criterion has proven effective and has yielded large samples of candidates with the SuperCOSMOS Sky Survey and Sloan Digital Sky Survey. In this work I will further increase the sample size with the Panchromatic Synoptic Telescope And Rapid Response System 1 (Pan–STARRS1). To construct luminosity functions for the study of the local white dwarfs, I require a density estimator that is generalised for a proper motion-limited sample. My simulations show that past works have underestimated the density when the tangential velocity was assumed to be a constant intrinsic parameter of an object. The intrinsically faint objects which are close to the upper proper motion limits of the surveys are most severely affected because of the poor approximation of a fixed tangential velocity. The survey volume is maximised by considering the small/intermediate scale variations in the observation properties at different epochs. This type of volume maximisation has not been conducted before because previous surveys did not have multi-epoch data over a footprint area of this size. The tessellation of the 3π Steradian Survey footprint is so complex that the variations are strong functions of position. I continue to demonstrate how a combination of a galactic model and the photometric limits as a function of position can give a good estimate of the completeness limits at different colour and different line-of-sight directions. Finally, I compare the derived white dwarf luminosity function with previous observational and theoretical work. The effect of interstellar reddening on the luminosity functions is also investigated.

Published
2016

4. Gamma-ray bursts in the local universe

Author

Chapman, Robert

Subjects
539.7222, Gamma-ray Burst, GRB, Magnetar, Neutron star, Soft Gamma Repeater, SGR, Neutron star binaries, Luminosity functions
Abstract

With energy outputs >~10^51 erg in 0.1-1000 seconds, Gamma-ray Bursts (GRBs) are the most powerful events yet observed in the Universe. As such they are potential probes of the very early Universe, back to the era of re-ionisation and the first stars, but at the same time they have been observed to span a wide range in luminosity and redshift from the relatively local Universe (z~0.0085) out to z~6.29. GRBs divide into two classes based primarily on their duration as measured by T90 (the time taken to observe 90% of the total burst fluence). Long bursts (L-GRBs) have T90>~2 seconds, and shorts (S-GRBs) T90<~2 seconds. Though much has been learned regarding long duration GRBs since the first afterglow discovery in 1997 (including their likely association with massive core collapse supernovae), much remains unknown regarding short duration GRBs. In this work, after a brief historical introduction and review, we present analyses of the angular cross-correlation on the sky of short GRBs from the BATSE catalogue with galaxies in the local Universe sampled from the PSCz Redshift Survey and the Third Reference Catalogue of Bright Galaxies (RC3). In particular we show that 20%+/-8% (1 sigma) of all BATSE short duration bursts (localised to 10 degrees or better) show correlation with galaxy samples (morphological T-type<=4) within ~112 Mpc. Our statistics thus provide evidence that a substantial fraction of BATSE short GRBs show a tendency to be associated with large scale structure on the sky traced by a variety of galaxy types. Short GRBs are believed to be produced in the final merger of compact object (neutron star-neutron star or neutron star-black hole) binaries, though other possible progenitors are known to exist. The short initial spike of a giant flare from a Soft Gamma Repeater (SGR) such as the December 27th 2004 event from SGR1806-20 would have been detectable by BATSE as a short GRB if it occurred in a galaxy within ~30-50 Mpc (assuming a distance to SGR1806-20 of 15 kpc). Using the observed luminosities and rates of Galactic SGR giant flares, as well as theoretical predictions for the rate of binary mergers, we investigate the ability of plausible Luminosity Functions (LF), singly and in combination, to reproduce our observed correlations and a cosmological S-GRB population. We find the correlations are best explained by a separate population of lower luminosity S-GRBs, with properties consistent with them being due to giant flares from extra-galactic SGRs. Overall predicted number counts are a good fit to the observed BATSE number counts, and furthermore, the wider redshift distribution is consistent with the early Swift S-GRB redshift distribution. The three closest GRBs which have been observed to date were all long duration bursts, and we have therefore also searched for cross-correlation signals between the BATSE long GRBs and local galaxies. The three nearby bursts shared several similar properties such as being under-luminous, spectrally soft and of low variability. We have therefore also investigated a subset of L-GRBs with light curve properties similar to these known nearby bursts. The whole sample is found to exhibit a correlation level consistent with zero (1 sigma upper limit=10%, equivalent to 144 bursts) out to a radius of ~155 Mpc, but a spectrally soft, low observed fluence and low variability subset shows a correlation level of 28%+/-16% (=50+/-28 bursts) within 155 Mpc. These results are consistent with low-luminosity, low-variability bursts being a separate sub-class of L-GRBs which may be much more prevalent in the local Universe than their high-luminosity, cosmologically distant counterparts. To investigate this further, we once again examined plausible luminosity functions for single and dual high and low luminosity populations, based on observed intrinsic rates from the literature. The local population was once again found only to be produced to a sufficient level (while maintaining consistency with the observed overall number counts) by a separate low luminosity population with intrinsic rates several hundred times greater than their cosmological counterparts. Constraining the models via the Swift overall redshift distribution instead of threshold-adjusted BATSE number counts showed that the dual LF models were able to produce excellent fits to the entire redshift distribution while adequately reproducing a local population. Finally, suggestions are made as to the direction future work may follow in order to build on these initial investigations, as well as to how observations with future missions and detectors such as Fermi (formerly GLAST), Advanced LIGO and LOFAR may shed further light on nearby GRBs.

Published
2009

5. Formation and evolution of dwarf early-type galaxies in the Virgo cluster II. Kinematic scaling relations

Author

Toloba, E., Boselli, A., Peletier, R. F., Falcón Barroso, J., van de Ven, G., Gorgas García, Francisco Javier, Toloba, E., Boselli, A., Peletier, R. F., Falcón Barroso, J., van de Ven, G., and Gorgas García, Francisco Javier

Abstract

© ESO, 2012. We thank the anonymous referee for his/her comments that have helped us to significantly improve this manuscript. E. T. thanks Juan Carlos Muñoz Mateos, Armando Gil de Paz, Mina Koleva, Sven de Rijcke, Puragra GuhaThakurta and Joshua Simon for very useful discussions. We thank the MAGPOP EU Marie Curie Training Network for financial support for the collaborating research visits and observations that allowed to make this paper. The observing time used in this work was part of the International Time Program (ITP 2005-2007, ITP4) at El Roque de los Muchachos Observatory (La Palma, Spain). E. T. thanks the financial support of the Fulbright Program jointly with the Spanish Ministry of Education. E. T. and J.G. have received financial support through the Spanish research projects AYA2007-67752-C03-03 and AYA2010-21322-C03-03. J.F.B. acknowledges support from the Ramón y Cajal Program as well as grant AYA2010-21322-C03-02 by the Spanish Ministry of Science and Innovation. This paper made use of the following public databases: SDSS (York et al. 2000), NASA/IPAC Extagalactic Database (NED, operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration), 2MASS (Two Micron All Sky Survey, Skrutskie et al. 2006, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation), HyperLEDA (Paturel et al. 2003), GOLDMine (Gavazzi et al. 2003)., We place our sample of 18 Virgo dwarf early-type galaxies (dEs) on the (V - K)_e-velocity dispersion, Faber-Jackson, and fundamental plane (FP) scaling relations for massive early-type galaxies (Es). We use a generalized velocity dispersion, which includes rotation, to be able to compare the location of both rotationally and pressure supported dEs with those of early and late-type galaxies. We find that dEs seem to bend the Faber-Jackson relation of Es to lower velocity dispersions, being the link between Es and dwarf spheroidal galaxies (dSphs). Regarding the FP relation, we find that dEs are significantly offset with respect to massive hot stellar systems, and re-casting the FP into the so-called.-space suggests that this offset is related to dEs having a total mass-to-light ratio higher than Es but still significantly lower than dSph galaxies. Given a stellar mass-to-light ratio based on the measured line indices of dEs, the FP offset allows us to infer that the dark matter fraction within the half light radii of dEs is on average ≳42% (uncertainties of 17% in the K band and 20% in the V band), fully consistent with an independent estimate in an earlier paper in this series. We also find that dEs in the size-luminosity relation in the near-infrared, like in the optical, are offset from early-type galaxies, but seem to be consistent with late-type galaxies. We thus conclude that the scaling relations show that dEs are different from Es, and that they further strengthen our previous findings that dEs are closer to and likely formed from late-type galaxies., Ministerio de Ciencia e Innovación (MCINN), Unión Europea. FP6, Fulbright Program, Ministerio de Educación, Cultura y Deporte (MECD), España, Programa Ramón y Cajal, Marie Curie Research Training Networks (UE), Marie Skłodowska-Curie Actions (UE), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2023

6. Kinematic properties as probes of the evolution of dwarf galaxies in the Virgo cluster

Author

Toloba, E., Boselli, A., Gorgas García, Francisco Javier, Peletier, R. F., Cenarro, A. J., Gadotti, D. A., Gil de Paz, Armando, Pedraz, S., Yildiz, U., Toloba, E., Boselli, A., Gorgas García, Francisco Javier, Peletier, R. F., Cenarro, A. J., Gadotti, D. A., Gil de Paz, Armando, Pedraz, S., and Yildiz, U.

Abstract

© 2009. The American Astronomical Society. All rights reserved. We thank the MAGPOP EU Marie Curie Training and Research Network for financial support and the anonymous referee for useful comments. E. T. and A. G. d. P. thank the Spanish research projects AYA2007-67752-C03-03 and AYA2006-02358, respectively. A. J. C. is Juan de la Cierva Fellow of the Spanish Ministry of Science and Innovation. This Letter made use of the following public databases: SDSS, NED, HyperLEDA ( Paturel et al. 2003), GOLDMine ( Gavazzi et al. 2003)., We present new observational results on the kinematical, morphological, and stellar population properties of a sample of 21 dEs located both in the Virgo Cluster and in the field, which show that 52% of the dEs (1) are rotationally supported, (2) exhibit structural signs of typical rotating systems such as disks, bars, or spiral arms, (3) are younger (~3 Gyr) than non-rotating dEs, and (4) are preferentially located either in the outskirts of Virgo or in the field. This evidence is consistent with the idea that rotationally supported dwarfs are late-type spirals or irregulars that recently entered the cluster and lost their gas through a ram pressure stripping event, quenching their star formation and becoming dEs through passive evolution. We also find that all, but one, galaxies without photometric hints for hosting disks are pressure supported and are all situated in the inner regions of the cluster. This suggests a different evolution from the rotationally supported systems. Three different scenarios for these non-rotating galaxies are discussed (in situ formation, harassment, and ram pressure stripping)., Unión Europea. FP6, Ministerio de Ciencia e Innovación (MICINN), Programa Juan de la Cierva (MICINN), Multi-wavelength analysis of galaxy populations (MAGPOP) Marie Curie Training and Research Network, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2023

7. Combining the CLAUDS and HSC-SSP surveys U plus grizy(+YJHK(s)) photometry and photometric redshifts for 18M galaxies in the 20 deg(2) of the HSC-SSP Deep and ultraDeep fields

Author

Desprez, G., Picouet, V., Moutard, T., Arnouts, S., Sawicki, M., Coupon, J., Gwyn, S., Chen, L., Huang, J., Golob, A., Furusawa, H., Ikeda, H., Paltani, S., Cheng, C., Hartley, W., Hsieh, B. C., Ilbert, O., Kauffmann, O. B., McCracken, H. J., Shuntov, M., Tanaka, M., Toft, S., Tresse, L., Weaver, J. R., Desprez, G., Picouet, V., Moutard, T., Arnouts, S., Sawicki, M., Coupon, J., Gwyn, S., Chen, L., Huang, J., Golob, A., Furusawa, H., Ikeda, H., Paltani, S., Cheng, C., Hartley, W., Hsieh, B. C., Ilbert, O., Kauffmann, O. B., McCracken, H. J., Shuntov, M., Tanaka, M., Toft, S., Tresse, L., and Weaver, J. R.

Abstract

We present the combination of the Canada-France-Hawaii Telescope (CHFT) Large Area U-bands Deep Survey (CLAUDS) and the Hyper-Suprime-Cam (HSC) Subaru Strategic Program (HSC-SSP) data over their four deep fields. We provide photometric catalogs for u, u* (CFHT-MegaCam), g, r, i, z, and y (Subaru-HSC) bands over similar to 20 deg(2), complemented in two fields by data from the Visible and Infrared Survey Telescope for Astronomy (VISTA) Deep Extragalactic Observations (VIDEO) survey and the UltraVISTA survey, thus extending the wavelength coverage toward near-infrared with VIRCAM Y, J, H, and K-s observations over 5.5 deg(2). The extraction of the photometry was performed with two different softwares: the HSC pipeline hscPipe and the standard and robust SExtractor software. Photometric redshifts were computed with template-fitting methods using the new Phosphoros code for the hscPipe photometry and the well-known Le Phare code for the SExtractor photometry. The products of these methods were compared with each other in detail. We assessed their quality using the large spectroscopic sample available in those regions, together with photometry and photometric redshifts from COSMOS2020, the latest version of the Cosmic Evolution Survey catalogs. We find that both photometric data sets are in good agreement in Ugrizy down to magnitude similar to 26, and to magnitude similar to 24.5 in the YJHK(s) bands. We achieve good performance for the photometric redshifts, reaching precisions of sigma(NMAD) less than or similar to 0.04 down to m(i) similar to 25, even using only the CLAUDS and HSC bands. At the same magnitude limit, we measured an outlier fraction of eta less than or similar to 10% when using the Ugrizy bands, and down to eta less than or similar to 6% when considering near-infrared data. The hscPipe plus Phosphoros pipeline performs slightly worse in terms of photometric-redshifts precision and outlier fraction than its SExtractor plus Le Phare counterpart, which

Published
2023

8. ALMACAL VIII:a pilot survey for untargeted extragalactic CO emission lines in deep ALMA calibration data

Author

Hamanowicz, Aleksandra, Zwaan, Martin A., Peroux, Celine, Lagos, Claudia del P., Klitsch, Anne, Ivison, Rob J., Biggs, Andrew D., Szakacs, Roland, Fresco, Alejandra, Hamanowicz, Aleksandra, Zwaan, Martin A., Peroux, Celine, Lagos, Claudia del P., Klitsch, Anne, Ivison, Rob J., Biggs, Andrew D., Szakacs, Roland, and Fresco, Alejandra

Abstract

We present a pilot, untargeted extragalactic carbon monoxide (CO) emission-line survey using ALMACAL, a project utilizing ALMA calibration data for scientific purposes. In 33 deep (T-exp' > 40 min) ALMACAL fields, we report six CO emission-line detections above S/N > 4, one-third confirmed by MUSE observations. With this pilot survey, we probe a cosmologically significant volume of similar to 10(5) cMpc(3), widely distributed over many pointings in the southern sky, making the survey largely insusceptible to the effects of cosmic variance. We derive the redshift probability of the CO detections using probability functions from the SHARK semi-analytical model of galaxy formation. By assuming typical CO excitations for the detections, we put constraints on the cosmic molecular gas mass density evolution over the redshift range 0 < z < 1.5. The results of our pilot survey are consistent with the findings of other untargeted emission-line surveys and the theoretical model predictions and currently cannot rule out a non-evolving molecular gas mass density. Our study demonstrates the potential of using ALMA calibrator fields as a multi-sightline untargeted CO emission-line survey. Applying this approach to the full ALMACAL database will provide an accurate, free of cosmic variance, measurement of the molecular luminosity function as a function of redshift.

Published
2023

9. ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE

Author

V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang, and Astronomy

Subjects
DECOMPOSITION, RED GALAXIES, Astronomy and Astrophysics, MASS, I, LUMINOSITY FUNCTIONS, Astrophysics - Astrophysics of Galaxies, EVOLUTION, STAR-FORMATION, Photometry, STELLAR, ULTRA-DEEP FIELD, Space and Planetary Science, Interstellar medium, Galaxy evolution, High-redshift galaxies, FRONTIER-FIELDS, Catalogs, Submillimeter astronomy
Abstract

We present a set of multiwavelength mosaics and photometric catalogs in the Atacama Large Millimeter/ submillimeter Array (ALMA) lensing cluster survey fields. The catalogs were built by the reprocessing of archival data from the Complete Hubble Archive for Galaxy Evolution compilation, taken by the Hubble Space Telescope (HST) in the Reionization Lensing Cluster Survey, Cluster Lensing And Supernova survey with Hubble, and Hubble Frontier Fields. Additionally, we have reconstructed the Spitzer Infrared Array Camera 3.6 and 4.5 μm mosaics, by utilizing all the available archival IPAC Infrared Science Archive/Spitzer Heritage Archive exposures. To alleviate the effect of blending in such a crowded region, we have modeled the Spitzer photometry by convolving the HST detection image with the Spitzer point-spread function using the novel GOLFIR software. The final catalogs contain 218,000 sources, covering a combined area of 690 arcmin2, a factor of ∼2 improvement over the currently existing photometry. A large number of detected sources is a result of reprocessing of all available and sometimes deeper exposures, in conjunction with a combined optical–near-IR detection strategy. These data will serve as an important tool in aiding the search of the submillimeter galaxies in future ALMA surveys, as well as follow-ups of the HST dark and high-z sources with JWST. Coupled with the available HST photometry, the addition of the 3.6 and 4.5 μm bands will allow us to place a better constraint on the photometric redshifts and stellar masses of these objects, thus giving us an opportunity to identify high-redshift candidates for spectroscopic follow-ups and to answer the important questions regarding the Epoch of Reionization and formation of the first galaxies. The mosaics, photometric catalogs, and the best-fit physical properties are publicly available at https:// github.com/dawn-cph/alcs-clusters., Danmarks Grundforskningsfond 140, Villum Fonden 13160 37440, Carlsberg Foundation CF18-0388, European Commission 896225 European Research Council (ERC) European Commission 648179, Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT) Japan Society for the Promotion of Science, Grants-in-Aid for Scientific Research (KAKENHI) JP17H06130, NAOJ ALMA Scientific Research 2017-06B, NRAO Student Observing Support (SOS) SOSPA7-022, Beatriz Galindo senior fellowship BG20/00224, Ministry of Science and Innovation, Spain (MICINN) PID2020-114414GB-100 PID2020-113689GB-I00, Junta de Andalucia P20_00334 FEDER/Junta de Andalucia-Consejeria de Transformacion Economica, Industria, Conocimiento y Universidades -FQM-510-UGR20, RELICS Treasury Program GO 14096, National Aeronautics & Space Administration (NASA) NAS5-26555

Published
2022
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10. CEERS Epoch 1 NIRCam Imaging: Reduction Methods and Simulations Enabling Early JWST Science Results

Author

Micaela B. Bagley, Steven L. Finkelstein, Anton M. Koekemoer, Henry C. Ferguson, Pablo Arrabal Haro, Mark Dickinson, Jeyhan S. Kartaltepe, Casey Papovich, Pablo G. Pérez-González, Nor Pirzkal, Rachel S. Somerville, Christopher N. A. Willmer, Guang Yang, L. Y. Aaron Yung, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Michaela Hirschmann, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Jennifer M. Lotz, Aubrey Medrano, Alexa M. Morales, Laura Pentericci, Swara Ravindranath, Jonathan R. Trump, Stephen M. Wilkins, Antonello Calabrò, M. C. Cooper, Luca Costantin, Alexander de la Vega, Bryan Hilbert, Taylor A. Hutchison, Rebecca L. Larson, Ray A. Lucas, Elizabeth J. McGrath, Russell Ryan, Xin Wang, and Stijn Wuyts

Subjects
semianalytic forecasts, survey design, space-telescope, massive galaxies, star-formation, synthetic nebular emission, light-cones, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, photometric catalogs, candels, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), luminosity functions, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We present the data release and data reduction process for the Epoch 1 NIRCam observations for the Cosmic Evolution Early Release Science Survey (CEERS). These data consist of NIRCam imaging in six broadband filters (F115W, F150W, F200W, F277W, F356W and F444W) and one medium band filter (F410M) over four pointings, obtained in parallel with primary CEERS MIRI observations (Yang et al. in prep). We reduced the NIRCam imaging with the JWST Calibration Pipeline, with custom modifications and reduction steps designed to address additional features and challenges with the data. Here we provide a detailed description of each step in our reduction and a discussion of future expected improvements. Our reduction process includes corrections for known pre-launch issues such as 1/f noise, as well as in-flight issues including snowballs, wisps, and astrometric alignment. Many of our custom reduction processes were first developed with pre-launch simulated NIRCam imaging over the full 10 CEERS NIRCam pointings. We present a description of the creation and reduction of this simulated dataset in the Appendix. We provide mosaics of the real images in a public release, as well as our reduction scripts with detailed explanations to allow users to reproduce our final data products. These represent one of the first official public datasets released from the Directors Discretionary Early Release Science (DD-ERS) program., 27 pages, 14 figures, submitted to ApJ. Accompanying CEERS public Data Release 0.5 available at ceers.github.io/releases.html

Published
2022
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11. ALMACAL VIII: A pilot survey for untargeted extragalactic CO emission lines in deep ALMA calibration data

Author

Aleksandra Hamanowicz, Martin A Zwaan, Céline Péroux, Claudia del P Lagos, Anne Klitsch, Rob J Ivison, Andrew D Biggs, Roland Szakacs, Alejandra Fresco, Laboratoire d'Astrophysique de Marseille (LAM), and 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)

Subjects
COSMIC EVOLUTION, SPECTROSCOPIC SURVEY, ISM [galaxies], INTERSTELLAR-MEDIUM, PHYSICAL-PROPERTIES, FOS: Physical sciences, Astronomy and Astrophysics, LUMINOSITY FUNCTIONS, Astrophysics - Astrophysics of Galaxies, ISM: molecules, star formation. [galaxies], STAR-FORMATION, BLIND SEARCH, galaxies: high-redshift, [SDU]Sciences of the Universe [physics], Space and Planetary Science, galaxies: star formation, Astrophysics of Galaxies (astro-ph.GA), MOLECULAR GAS CONTENT, GALAXY FORMATION, HIGH-REDSHIFT, galaxies: evolution, galaxies: ISM, molecules [ISM], evolution [galaxies]
Abstract

We present a pilot, untargeted extragalactic carbon monoxide (CO) emission-line survey using ALMACAL, a project utilizing ALMA calibration data for scientific purposes. In 33 deep (Texp > 40 min) ALMACAL fields, we report six CO emission-line detections above S/N > 4, one-third confirmed by MUSE observations. With this pilot survey, we probe a cosmologically significant volume of ∼105 cMpc3, widely distributed over many pointings in the southern sky, making the survey largely insusceptible to the effects of cosmic variance. We derive the redshift probability of the CO detections using probability functions from the Shark semi-analytical model of galaxy formation. By assuming typical CO excitations for the detections, we put constraints on the cosmic molecular gas mass density evolution over the redshift range 0 < z < 1.5. The results of our pilot survey are consistent with the findings of other untargeted emission-line surveys and the theoretical model predictions and currently cannot rule out a non-evolving molecular gas mass density. Our study demonstrates the potential of using ALMA calibrator fields as a multi-sightline untargeted CO emission-line survey. Applying this approach to the full ALMACAL database will provide an accurate, free of cosmic variance, measurement of the molecular luminosity function as a function of redshift.

Published
2022
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12. Emission line galaxies in the SHARDS Hubble frontier fields. II. Limits on Lyman-continuum escape fractions of lensed emission line galaxies at redshifts 2<z<3.5

Author

Alcalde Pampliega, Belén and Alcalde Pampliega, Belén

Abstract

© 2022. The Author(s). Artículo firmado por 13 autores. We thank the referee for comments that significantly improved the presentation of this paper. This work was supported by the Science and Technology Facilities Council in the form of a studentship to A.G. We also acknowledge support from the ERC Advanced Investigator Grant EPOCHS (788113). L.F. acknowledges funding from Coordenação de Aperfeiçoamento de Pessoal de Nível Superior—Brasil (CAPES)—Finance Code 001. D.C. is a Ramon-Cajal Researcher and is supported by the Ministerio de Ciencia, Innovación y Universidades (MICIU/FEDER) under research grant PGC2018-094975-C21. L.R.-M. acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001, and D.R.G. thanks CONACyT for research grant CB-A1-S-22784. This paper is (partly) based on SHARDS-FF data. SHARDS-FF is currently funded by Spanish Government grant PGC2018-093499-BI00. Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma. This work is also based partially on data and catalog products from HFF-DeepSpace, funded by the National Science Foundation and Space Telescope Science Institute (operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555). Software: galclean (Ferreira et al. 2018), astropy (Astropy Collaboration et al. 2013), FAST (Kriek et al. 2009), Scipy +Numpy (Virtanen et al. 2020), EAZY (Brammer et al. 2008), OSIRIS pipeline (Pérez-González et al. 2013)., the Science and Technology Facilities Council, the ERC Advanced Investigator, the Coordenação de Aperfeiçoamento de Pessoal de Nível Superior—Brasil (CAPES), Ministerio de Ciencia, Innovación y Universidades (MICIU/FEDER), the CONACyT, Gobierno de España, the National Science Foundation and Space Telescope Science Institute, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2022

13. This title is unavailable for guests, please login to see more information.

Author

Salvador Solé, Eduard, Manrique, Alberto, Mas Hesse, J. Miguel, Cabello González, Cristina, Gallego Maestro, Jesús, Rodríguez Espinosa, José Miguel, Guzmán, Rafael, Salvador Solé, Eduard, Manrique, Alberto, Mas Hesse, J. Miguel, Cabello González, Cristina, Gallego Maestro, Jesús, Rodríguez Espinosa, José Miguel, and Guzmán, Rafael

Abstract

© 2022. The Author(s). Funding for this work was provided by the Spanish MCIN/ AEI/10.13039/501100011033 under projects CEX2019-000918- M (Unidad de Excelencia “María de Maeztu” ICCUB), and PID2019-109361GB-100 (cofunded by FEDER funds), and the Catalan Department of Economy and Science grant 2017SGR643. J.M.M.-H. was funded by Spanish MICIN grants PID2019- 107061GB-C61 and MDM-2017-0737 (Unidad de Excelencia “María de Maeztu” Centro de Astrobiología). C.C. and J.G. were funded by Spanish MCIN grant AyA2018-rti-096188-b-i00, and J. M.R.-E. was funded by Spanish MCIN grant AYA2017-84061-P and the Canarian Government under project PROID2021010077. J.M.R.-E. is also indebted to the Severo Ochoa Program at the Instituto de Astrofísica de Canarias., Ministerio de Ciencia e Innovación (MCIN), FEDER funds, Catalan Department of Economy and Science, Gobierno de Canarias, Severo Ochoa Program at the Instituto de Astrofísica de Canarias, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2022

14. ALMA Lensing Cluster Survey:Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE

Author

Kokorev, Vasily, Brammer, G., Fujimoto, S., Kohno, K., Magdis, G. E., Valentino, F., Toft, S., Oesch, P., Davidzon, I., Bauer, F. E., Coe, D., Egami, E., Oguri, M., Ouchi, M., Postman, M., Richard, J., Jolly, J-B, Knudsen, K. K., Sun, F., Weaver, J. R., Ao, Y., Baker, A. J., Bradley, L., Caputi, K., Dessauges-Zavadsky, M., Espada, D., Hatsukade, B., Koekemoer, A. M., Arancibia, A. M. Munoz, Shimasaku, K., Umehata, H., Wang, T., Wang, W-H, Kokorev, Vasily, Brammer, G., Fujimoto, S., Kohno, K., Magdis, G. E., Valentino, F., Toft, S., Oesch, P., Davidzon, I., Bauer, F. E., Coe, D., Egami, E., Oguri, M., Ouchi, M., Postman, M., Richard, J., Jolly, J-B, Knudsen, K. K., Sun, F., Weaver, J. R., Ao, Y., Baker, A. J., Bradley, L., Caputi, K., Dessauges-Zavadsky, M., Espada, D., Hatsukade, B., Koekemoer, A. M., Arancibia, A. M. Munoz, Shimasaku, K., Umehata, H., Wang, T., and Wang, W-H

Abstract

We present a set of multiwavelength mosaics and photometric catalogs in the Atacama Large Millimeter/submillimeter Array (ALMA) lensing cluster survey fields. The catalogs were built by the reprocessing of archival data from the Complete Hubble Archive for Galaxy Evolution compilation, taken by the Hubble Space Telescope (HST) in the Reionization Lensing Cluster Survey, Cluster Lensing And Supernova survey with Hubble, and Hubble Frontier Fields. Additionally, we have reconstructed the Spitzer Infrared Array Camera 3.6 and 4.5 mu m mosaics, by utilizing all the available archival IPAC Infrared Science Archive/Spitzer Heritage Archive exposures. To alleviate the effect of blending in such a crowded region, we have modeled the Spitzer photometry by convolving the HST detection image with the Spitzer point-spread function using the novel GOLFIR software. The final catalogs contain 218,000 sources, covering a combined area of 690 arcmin(2) , a factor of similar to 2 improvement over the currently existing photometry. A large number of detected sources is a result of reprocessing of all available and sometimes deeper exposures, in conjunction with a combined optical-near-IR detection strategy. These data will serve as an important tool in aiding the search of the submillimeter galaxies in future ALMA surveys, as well as follow-ups of the HST dark and high-z sources with JWST. Coupled with the available HST photometry, the addition of the 3.6 and 4.5 mu m bands will allow us to place a better constraint on the photometric redshifts and stellar masses of these objects, thus giving us an opportunity to identify high-redshift candidates for spectroscopic follow-ups and to answer the important questions regarding the Epoch of Reionization and formation of the first galaxies. The mosaics, photometric catalogs, and the best-fit physical properties are publicly available at https:// github.com/dawn-cph/alcs-clusters.

Published
2022

15. Constraining the Hubble constant and its lower limit from the proper motion of extragalactic radio jets

Author

Hsiao, Tiger Yu-Yang, Goto, Tomotsugu, Hashimoto, Tetsuya, Santos, Daryl Joe D., Wong, Yi Hang Valerie, Kim, Seong Jin, Raquel, Bjorn Jasper R., Ho, Simon C-C, Chen, Bo-Han, Kilerci, Ece, Lu, Ting-Yi, On, Alvina Y. L., Lin, Yu-Wei, Wu, Cossas K-W, Hsiao, Tiger Yu-Yang, Goto, Tomotsugu, Hashimoto, Tetsuya, Santos, Daryl Joe D., Wong, Yi Hang Valerie, Kim, Seong Jin, Raquel, Bjorn Jasper R., Ho, Simon C-C, Chen, Bo-Han, Kilerci, Ece, Lu, Ting-Yi, On, Alvina Y. L., Lin, Yu-Wei, and Wu, Cossas K-W

Abstract

The Hubble constant (H-0) is a measurement to describe the expansion rate of the Universe in the current era. However, there is a 4.4 sigma discrepancy between the measurements from the early Universe and the late Universe. In this research, we propose a model-free and distance-free method to constrain H-0. Combining Friedman-Lemaltre-Robertson-Walker cosmology with geometrical relation of the proper motion of extragalactic jets, the lower limit (H-0,H-min) of H-0 can be determined using only three cosmology-free observables: the redshifts of the host galaxies, and the approaching and receding angular velocities of radio jets. Using these, we propose to use the Kolmogorov-Smirnov test (K-S test) between cumulative distribution functions of H-0,(min) to differentiate cosmology. We simulate 100, 200, and 500 extragalactic jets with three levels of accuracy of the proper motion (mu(a) and mu(r)), at 10, 5, and 1 per cent, corresponding to the accuracies of the current and future radio interferometers. We perform K-S tests between the simulated samples as theoretical distributions with different H-0 and power-law index of velocity distribution of jets and mock observational data. Our result suggests increasing sample sizes leads to tighter constraints on both power-law index and the Hubble constant at moderate accuracy (i.e. 10 and 5 per cent), while at 1 per cent accuracy, increasing sample sizes leads to tighter constraints on power-law index more. Improving accuracy results in better constraints in the Hubble constant compared with the power-law index in all cases, but it alleviates the degeneracy.

Published
2022

16. Forensic reconstruction of galaxy colour evolution and population characterization

Author

Bravo, Matias, Robotham, Aaron S. G., Lagos, Claudia del P., Davies, Luke J. M., Bellstedt, Sabine, Thorne, Jessica E., Bravo, Matias, Robotham, Aaron S. G., Lagos, Claudia del P., Davies, Luke J. M., Bellstedt, Sabine, and Thorne, Jessica E.

Abstract

Mapping the evolution of galaxy colours, from blue star forming to red passive systems, is fundamental to understand the processes involved in galaxy evolution. To this end, we reconstruct the colour evolution of low-redshift galaxies, combining stellar templates with star formation and metallicity histories of galaxies from the Galaxy And Mass Assembly survey and shark semi-analytical model. We use these colour histories to robustly characterize the evolution of red and blue galaxy populations over cosmic time. Using a Gaussian Mixture Model to characterize the colour distribution at any given epoch and stellar mass, we find both observations and simulations strongly favour a model with only two populations (blue and red), with no evidence for a third 'green' population. We map the evolution of mean, weight, and scatter of the blue and red populations as a function of both stellar mass and lookback time. Using our simulated galaxy catalogue as a testbed, we find that we can accurately recover galaxies colour histories up to a lookback time of similar to 6 Gyr. We find that both populations show little change in the mean colour for low-mass galaxies, while the colours at the massive end become significantly redder with time. The stellar mass above which the galaxy population is predominantly red decreases by 0.3 dex in the last 5 Gyrs. We find a good agreement between observations and simulations, with the largest tension being that massive galaxies from shark are too blue (a known issue with many galaxy evolution models).

Published
2022

17. A Gravitational-wave Measurement of the Hubble Constant Following the Second Observing Run of Advanced LIGO and Virgo

Author

G. Pagliaroli, Kevin Barkett, Denis Martynov, Marco Bazzan, C. Ingram, L. Pinard, Nicolas Sanchis-Gual, I. Belahcene, A. K. Y. Li, Archana Pai, F. Paoletti, P. Ruggi, G. Vajente, S. M. Gaebel, C. Kr mer, K. W. Chung, I. Dorrington, I. Di Palma, A. Mullavey, T. J. N. Nelson, Filip Morawski, Xiaohui Fan, Richard O'Shaughnessy, B. Barr, B. D. Lackey, G. Eddolls, A. Cumming, P. Grassia, Kipp Cannon, F. Di Renzo, M. Steinke, Francesco Pannarale, Soichiro Morisaki, D. Ugolini, P. Clearwater, M. Haney, T. A. Callister, Zhihui Du, G. Ciani, Alessandro Bertolini, Olivier Minazzoli, M. Razzano, Mairi Sakellariadou, G. Pillant, S. H. R. Yuen, O. de Varona, A. L. Stuver, R. De Rosa, I. Nardecchia, M. Kasprzack, J. Baird, Frances Hellman, M. B. Shaner, Manel Molina-Ruiz, S. B. Coughlin, Jessica Steinlechner, A. Neunzert, M. Heurs, Reed Essick, S. Kandhasamy, B. Sorazu, A. Kutynia, Andrea Chincarini, T. Z. Summerscales, Tenglin Li, Robert J. McCarthy, Linqing Wen, D. Meacher, Leo Tsukada, E. Z. Hamilton, A. Parida, S. S. Eikenberry, E. Genin, D. Estevez, W. Katzman, B. Grace, S. M. Aronson, M. Llorens-Monteagudo, M. Nery, Ryan Lynch, Ettore Majorana, D. M. Wilken, A. Rocchi, B. Goncharov, R. Birney, P. Ehrens, Paul M. Ricker, E. J. Fauchon-Jones, M. Lormand, William Parker, D. J. Stops, J. S. H. Lee, Felix Wellmann, Shreya Anand, D. Huet, S. H. Huttner, Z. Tornasi, Andrew Melatos, M. Lorenzini, M. Bitossi, J.-G. Ducoin, J. Neilson, G. Bergmann, K. Wette, John J. Oh, Timothy Evans, M. G. Benjamin, E. Payne, Rory Smith, C. Adams, R. M. Blair, D. Sigg, S. W. Ballmer, Z. Yang, D. M. Shoemaker, Michelle E. Walker, J. Eichholz, G. Moreno, H. Inchauspe, J. Liu, A. Pasqualetti, M. Tse, D. M. Macleod, B. L. Swinkels, J. Warner, R. Passaquieti, C. Rajan, O. Durante, N. Krupinski, F. Martelli, Karan Jani, Jade Powell, V. Mangano, H. K. Gulati, David H. Reitze, Rahul Kashyap, C. McIsaac, Nergis Mavalvala, A. K. Lenon, S. Mastrogiovanni, P. A. Altin, Piotr Jaranowski, Florent Robinet, J. Zhang, F. Baldaccini, L. F. Ortega, Jerome Degallaix, R. C. Walet, V. P. Mitrofanov, Rosa Poggiani, V. Frey, T. Sadecki, V. Tiwari, Yann Bouffanais, A. C. Green, C. Casentini, R. Shink, E. Goetz, F. Magaña-Sandoval, J. McIver, Sebastian Khan, B. C. Barish, J. H. Briggs, Mark Hannam, L. Rei, Gijs Nelemans, Tanja Hinderer, Alejandro Torres-Forné, A. K. Zadrożny, P.H. Nguyen, V. Boschi, E. J. Son, M. van Beuzekom, S. Grunewald, R. Prasanna, A. Ain, Shubhanshu Tiwari, G. A. Prodi, R. DeSalvo, V. Kondrashov, F. Frasconi, A. K. Mehta, E. D. Hall, S. Farinon, E. Mejuto Villa, D. Barker, A. Samajdar, Jolien D. E. Creighton, A. Pele, D. Singh, Arunava Mukherjee, Fausto Acernese, J. C. Barayoga, B. F. Neil, R. Flaminio, Richard J. Abbott, D. W. Yeeles, Hartmut Grote, D. C. Vander-Hyde, P. Puppo, W. Del Pozzo, Y. Minenkov, P. Bacon, P. F. Cohadon, H. Heitmann, A. Strunk, N. Kijbunchoo, Piero Rettegno, K. A. Santiago, P. J. Sutton, M. Cieślar, Maria Ilaria Del Principe, P. Raffai, J. C. Bayley, H. Wittel, M. Deenadayalan, G. H. Ogin, T. J. Shaffer, Marcus E. Lower, L. Glover, G. Losurdo, S. Biscoveanu, O. V. Palashov, Sean T. McWilliams, F. Piergiovanni, Chang-Hwan Lee, D. E. Cohen, M. Agathos, J. H. Romie, S. Sitmukhambetov, G. Kuehn, K. Merfeld, M. Ar ne, M. Phelps, Archisman Ghosh, R. G. Ormiston, Andrew Matas, A. Chiummo, K. Holt, M. Mantovani, E. A. Huerta, A. Ramos-Buades, S. L. Danilishin, Tristan Briant, R. K. Lanza, P. Dupej, Sheelu Abraham, Eric B. Flynn, J. Betzwieser, Antoine Heidmann, J. Hanks, A. Sur, H. Overmier, R. Goetz, Tarun Souradeep, J. P. Zendri, L. Sun, C. De Rossi, D. Buskulic, Odylio D. Aguiar, James Healy, P. Brockill, Luca Gammaitoni, R. Fittipaldi, C. Horst, Alberto Vecchio, F. Cipriano, Michael Thomas, R. Tenorio, N. A. Holland, D. Sellers, P. Popolizio, Koji Arai, F. J. Raab, Devon S. Johnson, N. Mukund, L. R. Cominsky, Neil J. Cornish, Colm Talbot, Andreas Freise, M. Davier, Sebastiano Bernuzzi, O. Halim, S. Koley, M. Brinkmann, C. Affeldt, S. Appert, Y. Setyawati, E. J. Sanchez, Nicholas Demos, J. D. Lough, D. Pascucci, H. S. Chen, L. E. H. Datrier, M. Bawaj, R. L. Savage, A. S. Bell, M. Laxen, Anchal Gupta, J. Meidam, M. Gosselin, Riccardo Sturani, M. K. M. Bader, O. Chaibi, Wolfango Plastino, R. Taylor, C. L. Romel, Giovanni Carapella, P. Shawhan, I. Ferrante, Soma Mukherjee, Charalampos Markakis, G. Mo, J. K. Blackburn, C. J. Richardson, F. L. Linde, E. Chassande-Mottin, Sylvain Marsat, Sheila Rowan, B. Gateley, Howard Pan, Aaron Buikema, R. Kirchhoff, B. L. Pearlstone, V. Fafone, Paul D. Lasky, R. K. Hasskew, Jordan Camp, D. Tao, M. Muratore, M. C. Heintze, D. Sentenac, F. Carbognani, Patrick Brady, P. Fulda, J. M. Fishner, Will M. Farr, M. Montani, Nancy Aggarwal, R. Gustafson, A. Grimaldi, J. W. Westhouse, Matthew Pitkin, F. Lin, Tania Regimbau, Serena Vinciguerra, F. Garufi, Chandra Kant Mishra, Joseph D. Romano, R. Bhandare, R. Pedurand, Benno Willke, C. C. Wipf, V. Pierro, M. J. Cowart, I. Dave, Lee McCuller, O. J. Piccinni, Takuya Tsutsui, T. D. Abbott, Zoheyr Doctor, M. Fletcher, B. Hughey, K. W. Tsang, P. J. Veitch, M. Rakhmanov, Surendra Nadh Somala, Gregorio Carullo, R. Xu, C. Buy, M. Oliver, Kazuhiro Agatsuma, T. J. Hansen, N. Bode, Christopher P. L. Berry, T. Harder, Rico K. L. Lo, P. Charlton, Kejia Lee, Patrick Das Gupta, S. E. Barclay, J. L. Willis, M. Eisenmann, Ofek Birnholtz, John A. Clark, Ben Farr, W. S. Kim, Christophe Collette, L. Kuo, H. Yamamoto, J. C. Driggers, A. Schönbeck, B. Rajbhandari, Daniel Wysocki, J. Prasad, A. J. Pedersen, S. B. Anderson, Tim Dietrich, M. Pürrer, S. Kwang, Frank Ohme, Vicky Kalogera, K. Rose, M. Tonelli, E. Katsavounidis, Xiuling Li, R. Gray, Patrick Godwin, M. C. Araya, Srishti Tiwari, S. Frasca, Jonathan Richardson, Tyson Littenberg, Kai Staats, L. Conti, M. Chaturvedi, Yu Huang, Geert Raaijmakers, F. Y. Khalili, R. P. Fisher, A. Allocca, D. I. Jones, Guoying Zhao, Kendall Ackley, R. K. Nayak, S. Raja, H. Y. Chia, Sascha Husa, S. E. Strigin, S. Mitra, M. Granata, H. J. Bulten, Minchuan Zhou, Shao-Jiang Wang, T. D. Creighton, S. E. Gossan, Dániel Barta, G. Venugopalan, Karl Gill, V. Srivastava, M. Fays, S. Barnum, S. C. Tait, K. Shukla, Zifan Zhou, I. A. Bilenko, L. Haegel, D.B. DeBra, David J. Ottaway, C. J. Perez, Matthew Evans, B. D. O'Brien, Marek Szczepanczyk, C. Bradaschia, M. Standke, Deep Jariwala, C. Cahillane, Otto A. Hannuksela, C. Gray, H. Estelles, W. A. Campbell, H. Radkins, A. Bozzi, N. N. Janthalur, L. Wallace, A. Królak, R. Frey, E. A. Muñiz, B. Sassolas, S. Brunett, Monica Colpi, Albino Perego, A. Bisht, M. Boer, J. B. Kanner, Andrew Lundgren, S. Xiao, J. V. Vanheijningen, D. Fiorucci, Zachariah B. Etienne, D. Moraru, E. Floden, Jennifer Watchi, A. K. Prajapati, Gianpietro Cagnoli, A. R. Wade, A. Di Lieto, S. J. Chamberlin, M. Vasúth, C. M. Mow-Lowry, Sergey P. Vyatchanin, Jonathan Cripe, V. Bossilkov, A. Paoli, Ik Siong Heng, A. Rüdiger, R. Inta, Steven Bloemen, Jonathan R. Gair, S. Klimenko, Eric Howell, E. Cesarini, S. Márka, N. Sennett, Stephen Fairhurst, Carl Blair, V. Fiumara, M. F. Carney, C. Lazzaro, Patricia Schmidt, Ajay Kumar, Y. K. Lecoeuche, M. J. Yap, C. Whittle, Bala R. Iyer, Stefan Grimm, D. B. Tanner, Kevin M. Ryan, S. McCormick, C. Difronzo, G. M. Harry, C. Palomba, S. Ascenzi, A. L. Miller, K. Venkateswara, L. Aiello, R. Green, Giuseppe Intini, Kenneth A. Strain, Jimin George, M. Sieniawska, Gregory Ashton, K. Chakravarti, G. Valdes, Ken K. Y. Ng, E. E. Cowan, B. D'Angelo, Hongyu Shen, D. C. Coyne, T. Dal Canton, J. Casanueva Diaz, P. Couvares, H. Fong, G. Greco, J. Zweizig, M. S. Shahriar, M. Korobko, J. Brooks, K. Siellez, Shiuh Chao, C. Périgois, P. Astone, Carlos O. Lousto, T. Hardwick, D. Steinmeyer, David Coward, A. Miani, R. Cotesta, Rakesh Kumar, F. Travasso, Yuri Levin, T. P. Downes, Gor Oganesyan, A. F. Brooks, P. J. Quinonez, Fabio Marchesoni, P. Hello, J. Gniesmer, Kyungmin Kim, Debarati Chatterjee, A. Trovato, B. O'Reilly, P. Gruning, Sheon Chua, R. Bonnand, C. North, Mariana Fazio, F. Vetrano, Samuele Cortese, Thomas Dent, P. Corban, S. J. Cooper, S. Leavey, Hai-Ping Cheng, A. Iess, M. Pedraza, M. Chan, Francesco Chiadini, Michał Bejger, Charlie Hoy, P. Schale, J. Jiang, J. Hennig, J. Junker, C. Van Den Broeck, E. Sowell, V. Gayathri, V. Hui, S. Walsh, Miriam Cabero, Alexander C. Jenkins, A. Markowitz, Robert Stone, M. Was, M. M. Hanke, G. Cho, James Whelan, P. Ajith, P. Booker, A. Perreca, G. Gemme, M. Drago, M. Di Giovanni, A. Malik, S. Gaudio, G. Dálya, T. Prestegard, J. Scott, L. K. Nuttall, A. W. Jones, Alessandro Nagar, R. De Pietri, Rocco Romano, M. Kinley-Hanlon, Lindsay DeMarchi, K. A. Thorne, E. L. Merilh, S. E. Dwyer, David Keitel, L. Matone, Mandar Patil, Guenakh Mitselmakher, B. A. Boom, A. M. Sergeev, Karsten Danzmann, A. R. Williamson, H. Vocca, Mario Spera, Peter Aufmuth, Andrea H. Tapia, Hua Wang, F. Cavalier, A. Bals, Yang Yang, S. G. Crowder, J. Bosveld, N. Koper, S. Kaufer, C. I. Torrie, Jan Harms, A. S. Sengupta, Xing-Jiang Zhu, Rana X. Adhikari, R. A. Mercer, S. Ossokine, Jinsook Kim, Om Sharan Salafia, C. K. Cheong, A. Lartaux-Vollard, M. Punturo, Leopoldo Milano, Slawomir Gras, L. Sammut, F. Muciaccia, Anupam Sharma, Lionel London, Moritz Mehmet, S. W. S. Ng, Suvadeep Bose, R. Gouaty, Debnandini Mukherjee, B. Idzkowski, V. Loriette, V. Skliris, R. Macas, G. Billingsley, S. Macfoy, Rainer Weiss, Alessandra Buonanno, R. Metzdorff, Isabel Cordero-Carrión, R. A. Eisenstein, Hee-Suk Cho, Gabrielle Allen, J.-M. Isac, B. Irwin, F. Donovan, S. Doravari, F. Ricci, W. Z. Korth, R. Kennedy, G. Fronz, F. Aubin, G. Stratta, László Á. Gergely, A. Macquet, Jishnu Suresh, G. D. Meadors, P. G. Murray, A. K. Divakarla, S. J. Kapadia, J. M. Gonzalez Castro, Z. Márka, Daichi Tsuna, Geoffrey Lovelace, M. Merzougui, Innocenzo M. Pinto, Haocun Yu, E. Biggs, L. Zhang, T. Zelenova, Riccardo Bassiri, Sebastian Steinlechner, C. A. Rose, X. Liu, Torrey Cullen, Magnus Manske, Bernard F. Whiting, Jesper Munch, Fabien Kéfélian, J. H. Hough, P. W. F. Forsyth, S. R. Thondapu, Chris A. Collins, Achamveedu Gopakumar, M. De Laurentis, M. Bischi, M. C. Milovich-Goff, J. L. Wright, J. R. Palamos, P. T. Baker, Carl-Johan Haster, Alessandra Corsi, D. Laghi, S. D'Antonio, E. Maros, P. B. Covas, L. Rolland, N. Letendre, B. D. Cheeseboro, B. Lantz, David Blair, P. J. Easter, K. Mogushi, Michele Zanolin, I. Magaña Hernandez, T. J. Massinger, Kiran Prasai, M. Khursheed, L. Naticchioni, D. Töyr, G. Vedovato, D. B. Kozak, F. Brighenti, Aniello Grado, D. Stocks, C. Vorvick, T. Vo, E. J. Daw, Salvatore Vitale, P. J. King, G. D. Hammond, K. H. Lai, Aaron Viets, Javed Rana, Abhirup Ghosh, G. Kang, A. L. Urban, Maurizio Canepa, J. Feicht, Satya Mohapatra, Antonio Marquina, L. Errico, T. A. Ferreira, K. D. Giardina, E. M. Santos, Nikhil Sarin, Martin Obergaulinger, M. Mondin, F. Marion, T. Huynh-Dinh, P. Weßels, Joey Shapiro Key, J. R. Sanders, C. F. Da Silva Costa, J. K. Wofford, Vuk Mandic, Chunglee Kim, M. A. Page, J. S. Kissel, H. Cao, D. J. Vine, R. M. S. Schofield, Fabrizio Barone, M. T. Hübner, N. Man, D. Lumaca, Benjamin J. Owen, J. F. J. van den Brand, J. S. Lange, M. A. Okada, E. Cuoco, Binlei Ding, S. Sunil, M. Tacca, Marta Colleoni, Bruno Giacomazzo, A. Gupta, Martin Hendry, Cecilio García-Quirós, J. A. Giaime, M. C. Tringali, K. Haughian, S. Hochheim, N. A. Robertson, D. Corre, Y. M. Kim, B. R. Hall, Maher Yazback, J. G. Bartlett, Márton Tápai, Marc Favata, Matteo Breschi, Fabrizio Bobba, Roger Jones, V. J. Roma, M. C. Díaz, Liam Cunningham, K. Mason, L. Trozzo, Antonios Kontos, S. A. Bilgili, E. C. Ferreira, Albert Lazzarini, A. P. Spencer, Sanjeev Dhurandhar, Jonathan Blackman, D. D. Brown, Anthony A. Amato, N. van Bakel, K. Toland, D. J. Hofman, A. Dmitriev, Samaya Nissanke, Y. Boetzel, S. Meshkov, Seog Oh, M. A. Bizouard, B. K. Berger, N. V. 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R, Pong, D, Ponrathnam, S, Popolizio, P, Porter, E, Powell, J, Prajapati, A, Prasad, J, Prasai, K, Prasanna, R, Pratten, G, Prestegard, T, Principe, M, Prodi, G, Prokhorov, L, Punturo, M, Puppo, P, Purrer, M, Qi, H, Quetschke, V, Quinonez, P, Raab, F, Raaijmakers, G, Radkins, H, Radulesco, N, Raffai, P, Raja, S, Rajan, C, Rajbhandari, B, Rakhmanov, M, Ramirez, K, Ramos-Buades, A, Rana, J, Rao, K, Rapagnani, P, Raymond, V, Razzano, M, Read, J, Regimbau, T, Rei, L, Reid, S, Reitze, D, Rettegno, P, Ricci, F, Richardson, C, Richardson, J, Ricker, P, Riemenschneider, G, Riles, K, Rizzo, M, Robertson, N, Robinet, F, Rocchi, A, Rolland, L, Rollins, J, Roma, V, Romanelli, M, Romano, J, Romano, R, Romel, C, Romie, J, Rose, C, Rose, D, Rose, K, Rosinska, D, Rosofsky, S, Ross, M, Rowan, S, Rudiger, A, Ruggi, P, Rutins, G, Ryan, K, Sachdev, S, Sadecki, T, Sakellariadou, M, Salafia, O, Salconi, L, Saleem, M, Samajdar, A, Sammut, L, Sanchez, E, Sanchez, L, Sanchis-Gual, N, Sanders, J, Santiago, K, Santos, E, Sarin, N, Sassolas, B, Sathyaprakash, B, Sauter, O, Savage, R, Schale, P, Scheel, M, Scheuer, J, Schmidt, P, Schnabel, R, Schofield, R, Schonbeck, A, Schreiber, E, Schulte, B, Schutz, B, Scott, J, Scott, S, Seidel, E, Sellers, D, Sengupta, A, Sennett, N, Sentenac, D, Sequino, V, Sergeev, A, Setyawati, Y, Shaddock, D, Shaffer, T, Shahriar, M, Shaner, M, Sharma, A, Sharma, P, Shawhan, P, Shen, H, Shink, R, Shoemaker, D, Shukla, K, Shyamsundar, S, Siellez, K, Sieniawska, M, Sigg, D, Singer, L, Singh, D, Singh, N, Singhal, A, Sintes, A, Sitmukhambetov, S, Skliris, V, Slagmolen, B, Slaven-Blair, T, Smith, J, Smith, R, Somala, S, Son, E, Soni, S, Sorazu, B, Sorrentino, F, Souradeep, T, Sowell, E, Spencer, A, Spera, M, Srivastava, A, Srivastava, V, Staats, K, Stachie, C, Standke, M, Steer, D, Steinke, M, Steinlechner, J, Steinlechner, S, Steinmeyer, D, Stevenson, S, Stocks, D, Stone, R, Stops, D, Strain, K, Stratta, G, Strigin, S, Strunk, A, Sturani, R, Stuver, A, Sudhir, V, Summerscales, T, Sun, L, Sunil, S, Sur, A, Suresh, J, Sutton, P, Swinkels, B, Szczepanczyk, M, Tacca, M, Tait, S, Talbot, C, Tanner, D, Tao, D, Tapai, M, Tapia, A, Tasson, J, Taylor, R, Tenorio, R, Terkowski, L, Thomas, M, Thomas, P, Thondapu, S, Thorne, K, Thrane, E, Tiwari, S, Tiwari, V, Toland, K, Tonelli, M, Tornasi, Z, Torres-Forne, A, Torrie, C, Toyr, D, Travasso, F, Traylor, G, Tringali, M, Tripathee, A, Trovato, A, Trozzo, L, Tsang, K, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tsutsui, T, Tuyenbayev, D, Ueno, K, Ugolini, D, Unnikrishnan, C, Urban, A, Usman, S, Vahlbruch, H, Vajente, G, Valdes, G, Valentini, M, Bakel, N, Beuzekom, M, Brand, J, Broeck, C, Vander-Hyde, D, Schaaf, L, Vanheijningen, J, Veggel, A, Vardaro, M, Varma, V, Vass, S, Vasuth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venkateswara, K, Venugopalan, G, Verkindt, D, Vetrano, F, Vicere, A, Viets, A, Vinciguerra, S, Vine, D, Vinet, J, Vitale, S, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, S, Wade, A, Wade, L, Wade, M, Walet, R, Walker, M, Wallace, L, Walsh, S, Wang, H, Wang, J, Wang, S, Wang, W, Wang, Y, Ward, R, Warden, Z, Warner, J, Was, M, Watchi, J, Weaver, B, Wei, L, Weinert, M, Weinstein, A, Weiss, R, Wellmann, F, Wen, L, Wessel, E, Wessels, P, Westhouse, J, Wette, K, Whelan, J, Whiting, B, Whittle, C, Wilken, D, Williams, D, Williamson, A, Willis, J, Willke, B, Winkler, W, Wipf, C, Wittel, H, Woan, G, Woehler, J, Wofford, J, Wright, J, Wu, D, Wysocki, D, Xiao, S, Xu, R, Yamamoto, H, Yancey, C, Yang, L, Yang, Y, Yang, Z, Yap, M, Yazback, M, Yeeles, D, Yu, H, Yuen, S, Zadrozny, A, Zanolin, M, Zelenova, T, Zendri, J, Zevin, M, Zhang, J, Zhang, L, Zhang, T, Zhao, C, Zhao, G, Zhou, M, Zhou, Z, Zhu, X, Zimmerman, A, Zucker, M, Zweizig, J, Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique 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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), Institut des Fonctions Optiques pour les Technologies de l'informatiON (Institut FOTON), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-Université Bretagne Loire (UBL)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut 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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 d'Annecy de Physique des Particules (LAPP), Université Nice Sophia Antipolis (1965 - 2019) (UNS), 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 de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-École 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Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution)), Spectroscopies optiques des matériaux verres, amorphes et à nanoparticules (SOPRANO), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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), LIGO Scientific Collaboration, Virgo Collaboration, Arène, M., Bécsy, B., Bustillo, J. Calderón, Diaz, J. Casanueva, Cavaglià, M., Cerdá-Durán, P., Cieślar, M., Cordero-Carrión, I., Dálya, G., D’Angelo, B., D’Antonio, S., Deléglise, S., Pozzo, W. Del, de Varona, O., Díaz, M. C., Vivanco, Francisco Hernandez, Fronzè, G., García-Quirós, C., Ghosh, Abhirup, Ghosh, Archisman, González, G., Gupta, Anchal, Hübner, M. T., Kéfélian, F., Kim, Chunglee, Krämer, C., Królak, A., Kumar, Rahul, Kumar, Rakesh, Lück, H., Hernandez, I. Magaña, Magaña-Sandoval, F., Márka, S., Márka, Z., Villa, E. Mejuto, Mukherjee, Arunava, Mukherjee, Subroto, Muñiz, E. A., O’Brien, B. D., Oram, Richard J., O’Reilly, B., O’Shaughnessy, R., Périgois, C., Pinto, I. M., Pürrer, M., Rana, Javed, Rosińska, D., Rüdiger, A., Schönbeck, A., Szczepańczyk, M. J., Tápai, M., Tiwari, Shubhanshu, Tiwari, Srishti, Torres-Forné, A., Töyrä, D., Bakel, N. van, Beuzekom, M. van, Brand, J. F. J. van den, Broeck, C. Van Den, Schaaf, L. van der, Veggel, A. A. van, Vasúth, M., Viceré, A., Weßels, P., Yu, Hang, Yu, Haocun, Zadrożny, A. K., Zadrożny, A., RS: FSE MSP, Grav. waves and fundamental physics, RS: FSE Grav. waves and fundamental physics, Faculty of Science, Gravitation and Astroparticle Physics Amsterdam, Other Research IHEF (IoP, FNWI), IoP (FNWI), and Astroparticle Physics (IHEF, IoP, FNWI)

Subjects
Gravitació, neutron star: binary, cosmological model, 010504 meteorology & atmospheric sciences, Astronomy, Gravitational Waves, Hubble constant, O2, LIGO, Virgo, detector: network, 01 natural sciences, Cosmology, General Relativity and Quantum Cosmology, LIGO, dark energy, 010303 astronomy & astrophysics, QC, Physics, Settore FIS/01, Hubble constant, Settore FIS/05, CATALOG, Physical Sciences, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), DATA RELEASE, COSMOLOGICAL PARAMETERS, FOS: Physical sciences, O2, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, LUMINOSITY FUNCTIONS, gravitational radiation: direct detection, Gravitational-wave astronomy, 1ST, Article, electromagnetic field: production, symbols.namesake, Binary black hole, 0103 physical sciences, DISTRIBUTIONS, K-CORRECTIONS, SDG 7 - Affordable and Clean Energy, Astrophysique, STFC, 0105 earth and related environmental sciences, Gravitational Waves, Science & Technology, Gravitational wave, Virgo, RCUK, Astronomy and Astrophysics, cosmology, gravitational waves, 310 Galaxies and Cosmology, Galaxy, EVOLUTION, Dewey Decimal Classification::500 | Naturwissenschaften::520 | Astronomie, Kartographie, gravitational radiation detector, VIRGO, black hole: binary, Space and Planetary Science, [SDU]Sciences of the Universe [physics], DENSITY, gravitational radiation: emission, Dark energy, Astronomia, ddc:520, galaxy, Gravitational wave astronomy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law
Abstract

This paper presents the gravitational-wave measurement of the Hubble constant (H 0) using the detections from the first and second observing runs of the Advanced LIGO and Virgo detector network. The presence of the transient electromagnetic counterpart of the binary neutron star GW170817 led to the first standard-siren measurement of H 0. Here we additionally use binary black hole detections in conjunction with galaxy catalogs and report a joint measurement. Our updated measurement is H 0 = km s-1 Mpc-1 (68.3% of the highest density posterior interval with a flat-in-log prior) which is an improvement by a factor of 1.04 (about 4%) over the GW170817-only value of km s-1 Mpc-1. A significant additional contribution currently comes from GW170814, a loud and well-localized detection from a part of the sky thoroughly covered by the Dark Energy Survey. With numerous detections anticipated over the upcoming years, an exhaustive understanding of other systematic effects are also going to become increasingly important. These results establish the path to cosmology using gravitational-wave observations with and without transient electromagnetic counterparts., 0, info:eu-repo/semantics/published

Published
2021
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18. Modeling of radio source counts as function of radiation flow

Author

Pendo, Pero and Smolčić, Vernesa

Subjects
PRIRODNE ZNANOSTI. Fizika, funkcije luminoziteta, aktivne galaktičke jezgre, active galactic nuclei, galaksije s povećanom brzinom nastanka zvijezda, diferencijalni brojevi izvora, luminosity functions, star-forming galaxies, NATURAL SCIENCES. Physics, differential source counts
Abstract

U radiovalnom području detektirano zračenje galaksija uvelike je sinkrotronsko zračenje koje nastaje kada se nabijene čestice gibaju relativističkim brzinama unutar magnetskog polja. S obzirom na proces koji uzrokuje ovo zračenje, izvori se mogu podijeliti na dvije skupine. Prva skupina su galaksije koje u svom središtu posjeduju aktivnu galaktičku jezgru (AGN galaksije). Druga skupina su galaksije s povećanom brzinom nastanka zvijezda (SF galaksije). Obje skupine izvora se detektiraju radiopregledima neba te se bilježe u kataloge izvora. Najjednostavniji način obrade podataka iz kataloga je brojanje izvora. Diferencijalni broj izvora definiran je kao broj izvora po gustoći toka zračenja po prostornom kutu. Diferencijalni broj izvora može se dobiti i iz funkcija luminoziteta. Funkcije luminoziteta daju brojčanu gustoću objekata unutar određenog intervala luminoziteta. Funkcije luminoziteta ovise o vrijednosti kozmološkog crvenog pomaka i kažemo da evoluiraju. U ovom radu se iz postojećih analitičkih modela evolucije funkcija luminoziteta računaju diferencijalni brojevi izvora za dvije spomenute populacije. Također, diferencijalni brojevi izvora se računaju i iz podataka preuzetih iz raznih kataloga. Rezultati dobiveni iz analitičkih modela i podataka slažu se unutar nepouzdanosti računa. Na najvećim vrijednostima toka zračenja brojem izvora dominiraju AGN galaksije. Podjednak doprinos broju izvora od obje populacije nalazi se na vrijednostima toka zračenja od 200 μJy. Na vrijednostima toka zračenja ispod 10 μJy udio SF galaksija je veći od 90% te one dominiraju diferencijalnim brojem izvora u ovom području. Detected radio emission from galaxies is largely synchrotron emission, which is created when charged particles move with relativistic velocities inside a magnetic field. Depending on the process that is causing this emission, sources can be separated into two distinct populations. The first population are galaxies that have active galactic nuclei (AGN galaxies). The second population are star-forming galaxies (SF). Both populations are detected via radio sky surveys and categorized in source catalogues. The easiest way to process data from a catalogue is simply counting the sources. Differential source counts are defined as number of sources per unit flux density per unit solid angle. Differential source counts can also be obtained from luminosity functions. Luminosity functions give the number density of objects inside a predefined interval of luminosity. Luminosity functions depend on the cosmological redshift and it can be said that they evolve. In this paper, differential source counts for two previously mentioned populations are obtained using predefined analytical models of evolving luminosity functions. Differential source counts are also obtained from data taken from various catalogues. Results obtained from analytical models and from data are well constrained within the uncertainty of the calculation. Differential source counts are dominated by AGN galaxies at highest values of flux density. Equal contribution to the differential source counts from both types of sources is found at flux density values of 200 μJy. Below 10 μJy the fraction of SF galaxies is higher than 90% as they dominate differential source counts at these values of flux density.

Published
2022

19. Constraining the Hubble constant and its lower limit from the proper motion of extragalactic radio jets

Author

Tiger Yu-Yang Hsiao, Tomotsugu Goto, Tetsuya Hashimoto, Daryl Joe D Santos, Yi Hang Valerie Wong, Seong Jin Kim, Bjorn Jasper R Raquel, Simon C-C Ho, Bo-Han Chen, Ece Kilerci, Ting-Yi Lu, Alvina Y L On, Yu-Wei Lin, and Cossas K-W Wu

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), jets [galaxies], FOS: Physical sciences, MOJAVE, Astronomy and Astrophysics, VELOCITY, LUMINOSITY FUNCTIONS, Astrophysics - Astrophysics of Galaxies, INTRINSIC-PROPERTIES, GALAXIES, VLBA EXPERIMENTS, proper motions, GHZ, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), DISTANCE, RELATIVISTIC JETS, KINEMATICS, cosmological parameters, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Hubble constant ($H_{0}$) is a measurement to describe the expansion rate of the Universe in the current era. However, there is a $4.4\sigma$ discrepancy between the measurements from the early Universe and the late Universe. In this research, we propose a model-free and distance-free method to constrain $H_{0}$. Combining Friedman-Lema\^itre-Robertson-Walker cosmology with geometrical relation of the proper motion of extragalactic jets, the lower limit ($H_{\rm 0,min}$) of $H_{0}$ can be determined using only three cosmology-free observables: the redshifts of the host galaxies, as well as the approaching and receding angular velocities of radio jets. Using these, we propose to use the Kolmogorov-Smirnov test (K-S test) between cumulative distribution functions of $H_{\rm 0,min}$ to differentiate cosmology. We simulate 100, 200, and 500 extragalactic jets with 3 levels of accuracy of the proper motion ($\mu_{a}$ and $\mu_{r}$), at $10\%$, $5\%$, and $1\%$, corresponding to the accuracies of the current and future radio interferometers. We perform K-S tests between the simulated samples as theoretical distributions with different $H_{0}$ and power-law index of velocity distribution of jets and mock observational data. Our result suggests increasing sample sizes leads to tighter constraints on both power-law index and the Hubble constant at moderate accuracy (i.e., $10\%$ and $5\%$) while at $1\%$ accuracy, increasing sample sizes leads to tighter constraints on power-law index more. Improving accuracy results in better constraints in the Hubble constant compared with the power-law index in all cases but it alleviates the degeneracy., Comment: 13 pages, 14 figures, accepted for publication in MNRAS

Published
2022
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20. Search for High-energy Neutrinos from Ultraluminous Infrared Galaxies with IceCube

Author

IceCube Collaboration, Abbasi, R., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Alispach, C., Alves, A. A., Amin, N. M., An, R., Andeen, K., Anderson, T., Anton, G., Arg��elles, C., Ashida, Y., Axani, S., Bai, X., V., A. Balagopal, Barbano, A., Barwick, S. W., Bastian, B., Basu, V., Baur, S., Bay, R., Beatty, J. J., Becker, K. -H., Tjus, J. Becker, Bellenghi, C., BenZvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Boddenberg, M., Bontempo, F., Borowka, J., B��ser, S., Botner, O., B��ttcher, J., Bourbeau, E., Bradascio, F., Braun, J., Bron, S., Brostean-Kaiser, J., Browne, S., Burgman, A., Burley, R. T., Busse, R. S., Campana, M. A., Carnie-Bronca, E. G., Chen, C., Chirkin, D., Choi, K., Clark, B. A., Clark, K., Classen, L., Coleman, A., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dappen, C., Dave, P., De Clercq, C., DeLaunay, J. J., Dembinski, H., Deoskar, K., De Ridder, S., Desai, A., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., DeYoung, T., Dharani, S., Diaz, A., D��az-V��lez, J. C., Dittmer, M., Dujmovic, H., Dunkman, M., DuVernois, M. A., Dvorak, E., Ehrhardt, T., Eller, P., Engel, R., Erpenbeck, H., Evans, J., Evenson, P. A., Fan, K. L., Fazely, A. R., Fiedlschuster, S., Fienberg, A. T., Filimonov, K., Finley, C., Fischer, L., Fox, D., Franckowiak, A., Friedman, E., Fritz, A., F��rst, P., Gaisser, T. K., Gallagher, J., Ganster, E., Garcia, A., Garrappa, S., Gerhardt, L., Ghadimi, A., Glaser, C., Glauch, T., Gl��senkamp, T., Goldschmidt, A., Gonzalez, J. G., Goswami, S., Grant, D., Gr��goire, T., Griswold, S., G��nd��z, M., G��nther, C., Haack, C., Hallgren, A., Halliday, R., Halve, L., Halzen, F., Minh, M. Ha, Hanson, K., Hardin, J., Harnisch, A. A., Haungs, A., Hauser, S., Hebecker, D., Helbing, K., Henningsen, F., Hettinger, E. C., Hickford, S., Hignight, J., Hill, C., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Huber, T., Hultqvist, K., H��nnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jansson, M., Japaridze, G. S., Jeong, M., Jones, B. J. P., Kang, D., Kang, W., Kang, X., Kappes, A., Kappesser, D., Karg, T., Karl, M., Karle, A., Katz, U., Kauer, M., Kellermann, M., Kelley, J. L., Kheirandish, A., Kin, K., Kintscher, T., Kiryluk, J., Klein, S. R., Koirala, R., Kolanoski, H., Kontrimas, T., K��pke, L., Kopper, C., Kopper, S., Koskinen, D. J., Koundal, P., Kovacevich, M., Kowalski, M., Kozynets, T., Kun, E., Kurahashi, N., Lad, N., Gualda, C. Lagunas, Lanfranchi, J. L., Larson, M. J., Lauber, F., Lazar, J. P., Lee, J. W., Leonard, K., Leszczy��ska, A., Li, Y., Lincetto, M., Liu, Q. R., Liubarska, M., Lohfink, E., Mariscal, C. J. Lozano, Lu, L., Lucarelli, F., Ludwig, A., Luszczak, W., Lyu, Y., Ma, W. Y., Madsen, J., Mahn, K. B. M., Makino, Y., Mancina, S., Mari{��}, I. C., Maruyama, R., Mase, K., McElroy, T., McNally, F., Mead, J. V., Meagher, K., Medina, A., Meier, M., Meighen-Berger, S., Micallef, J., Mockler, D., Montaruli, T., Moore, R. W., Morse, R., Moulai, M., Naab, R., Nagai, R., Naumann, U., Necker, J., Nguy{\~{��}}n, L. V., Niederhausen, H., Nisa, M. U., Nowicki, S. C., Nygren, D. R., Pollmann, A. Obertacke, Oehler, M., Olivas, A., O'Sullivan, E., Pandya, H., Pankova, D. V., Park, N., Parker, G. K., Paudel, E. N., Paul, L., Heros, C. P��rez de los, Peters, L., Peterson, J., Philippen, S., Pieloth, D., Pieper, S., Pittermann, M., Pizzuto, A., Plum, M., Popovych, Y., Porcelli, A., Rodriguez, M. Prado, Price, P. B., Pries, B., Przybylski, G. T., Raab, C., Raissi, A., Rameez, M., Rawlins, K., Rea, I. C., Rehman, A., Reichherzer, P., Reimann, R., Renzi, G., Resconi, E., Reusch, S., Rhode, W., Richman, M., Riedel, B., Roberts, E. J., Robertson, S., Roellinghoff, G., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Cantu, D. Rysewyk, Safa, I., Saffer, J., Herrera, S. E. Sanchez, Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Scharf, M., Schaufel, M., Schieler, H., Schindler, S., Schlunder, P., Schmidt, T., Schneider, A., Schneider, J., Schr��der, F. G., Schumacher, L., Schwefer, G., Sclafani, S., Seckel, D., Seunarine, S., Sharma, A., Shefali, S., Silva, M., Skrzypek, B., Smithers, B., Snihur, R., Soedingrekso, J., Soldin, D., Spannfellner, C., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., St��rwald, T., Stuttard, T., Sullivan, G. W., Taboada, I., Tenholt, F., Ter-Antonyan, S., Tilav, S., Tischbein, F., Tollefson, K., Tomankova, L., T��nnis, C., Toscano, S., Tosi, D., Trettin, A., Tselengidou, M., Tung, C. F., Turcati, A., Turcotte, R., Turley, C. F., Twagirayezu, J. P., Ty, B., Elorrieta, M. A. Unland, Valtonen-Mattila, N., Vandenbroucke, J., van Eijndhoven, N., Vannerom, D., van Santen, J., Verpoest, S., Vraeghe, M., Walck, C., Watson, T. B., Weaver, C., Weigel, P., Weindl, A., Weiss, M. J., Weldert, J., Wendt, C., Werthebach, J., Weyrauch, M., Whitehorn, N., Wiebusch, C. H., Williams, D. R., Wolf, M., Woschnagg, K., Wrede, G., Wulff, J., Xu, X. W., Xu, Y., Yanez, J. P., Yoshida, S., Yu, S., Yuan, T., Zhang, Z., Physics, Faculty of Sciences and Bioengineering Sciences, Vriendenkring VUB, and Elementary Particle Physics

Subjects
ACTIVE GALACTIC NUCLEI, FLUX, TELESCOPE, neutrino: energy: high, Astrophysics::High Energy Astrophysical Phenomena, pole, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, LUMINOSITY FUNCTIONS, 7. Clean energy, neutrino: flux, IceCube, Astronomi, astrofysik och kosmologi, formation [star], JY SAMPLE, Astronomy, Astrophysics and Cosmology, TeV, ddc:530, energy: high [neutrino], AGN, Astrophysics::Galaxy Astrophysics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), background, Physics, High Energy Physics::Phenomenology, Astronomy and Astrophysics, flux [neutrino], star: formation, redshift, STAR-FORMATION HISTORY, EVOLUTION, ddc, observatory, Physics and Astronomy, 13. Climate action, Space and Planetary Science, stacking, infrared, STARBURST, ddc:520, High Energy Physics::Experiment, galaxy, Astrophysics - High Energy Astrophysical Phenomena, OPTICAL SPECTROSCOPY
Abstract

The astrophysical journal 926(1), 59 (2022). doi:10.3847/1538-4357/ac3cb6, Ultraluminous infrared galaxies (ULIRGs) have infrared luminosities L $_{IR}$ ��� 10$^{12}$ L $_{���}$, making them the most luminous objects in the infrared sky. These dusty objects are generally powered by starbursts with star formation rates that exceed 100 M $_{���}$ yr$^{���1}$, possibly combined with a contribution from an active galactic nucleus. Such environments make ULIRGs plausible sources of astrophysical high-energy neutrinos, which can be observed by the IceCube Neutrino Observatory at the South Pole. We present a stacking search for high-energy neutrinos from a representative sample of 75 ULIRGs with redshift z ��� 0.13 using 7.5 yr of IceCube data. The results are consistent with a background-only observation, yielding upper limits on the neutrino flux from these 75 ULIRGs. For an unbroken E $^{���2.5}$ power-law spectrum, we report an upper limit on the stacked flux at 90% confidence level. In addition, we constrain the contribution of the ULIRG source population to the observed diffuse astrophysical neutrino flux as well as model predictions., Published by Univ., Chicago, Ill. [u.a.]

Published
2022
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22. Measuring the H i Content of Individual Galaxies Out to the Epoch of Reionization with [C ii]

Author

Heintz, Kasper E., Watson, Darach, Oesch, Pascal A., Narayanan, Desika, Madden, Suzanne C., Heintz, Kasper E., Watson, Darach, Oesch, Pascal A., Narayanan, Desika, and Madden, Suzanne C.

Abstract

The H i gas content is a key ingredient in galaxy evolution, the study of which has been limited to moderate cosmological distances for individual galaxies due to the weakness of the hyperfine H i 21 cm transition. Here we present a new approach that allows us to infer the H i gas mass M (HI) of individual galaxies up to z approximate to 6, based on a direct measurement of the [C ii]-to-H i conversion factor in star-forming galaxies at z greater than or similar to 2 using gamma-ray burst afterglows. By compiling recent [C ii]-158 mu m emission line measurements we quantify the evolution of the H i content in galaxies through cosmic time. We find that M (HI) starts to exceed the stellar mass M at z greater than or similar to 1, and increases as a function of redshift. The H i fraction of the total baryonic mass increases from around 20% at z = 0 to about 60% at z similar to 6. We further uncover a universal relation between the H i gas fraction M (HI)/M and the gas-phase metallicity, which seems to hold from z approximate to 6 to z = 0. The majority of galaxies at z > 2 are observed to have H i depletion times, t (dep,HI) = M (HI)/SFR, less than approximate to 2 Gyr, substantially shorter than for z similar to 0 galaxies. Finally, we use the [C ii]-to-H i conversion factor to determine the cosmic mass density of H i in galaxies, rho (HI), at three distinct epochs: z approximate to 0, z approximate to 2, and z similar to 4-6. These measurements are consistent with previous estimates based on 21 cm H i observations in the local universe and with damped Ly alpha absorbers (DLAs) at z greater than or similar to 2, suggesting an overall decrease by a factor of approximate to 5 in rho (HI)(z) from the end of the reionization epoch to the present.

Published
2021

23. A Radio Measurement of the Star Formation History of the Universe

Subjects
Astrophysics::High Energy Astrophysical Phenomena, galaxy evolution, cosmological evolution, active galaxies, Astrophysics::Cosmology and Extragalactic Astrophysics, luminosity functions, Astrophysics::Galaxy Astrophysics, star formation
Abstract

Most of the stars in the universe were formed by disk galaxies like our own Milky Way during an era poetically called “cosmic noon.” This era, occurring approximately 3 billion years after the Big Bang, marked the peak of not only star formation, but also black hole growth and dust attenuation. The dust that permeates all galaxies absorbs and scatters the ultraviolet and optical light primarily generated by massive stars, whose lives are so short that they provide an effectively instantaneous measurement of the star formation rate. Understanding the formation and evolution of galaxies at cosmic noon is essential to understanding how the universe appears and acts today---but the uncertainties imposed by dust are worst during this influential period. Radio emission is entirely unaffected by dust and is generated by supernova remnants of the same massive stars emitting primarily in the UV and optical. Radio observations of star-forming galaxies are therefore a powerful tracer of star formation rate, but it has not been until the past decade that radio observations have been sensitive enough to detect Milky Way-like galaxies at cosmic noon. In this dissertation, I calculate and combine the source counts from the deepest radio continuum image to date with the local luminosity function of radio sources to model the star formation history of the universe. I determined the local luminosity functions for both star-forming galaxies (SFGs) and active galactic nuclei (AGNs) using N ~ 10,000 radio sources from the NRAO VLA Sky Survey (NVSS) cross-identified with galaxies in the 2MASS Extended (2MASX) catalog (Chapter 2). The AGNs and SFGs were separated using only radio and infrared data rather than optical emission-line diagnostics, which are not good quantitative measures of AGN-powered radio emission. Our sample of radio sources account for >99% of the total 1.4 GHz energy density in the nearby universe. The local radio-derived star formation rate density (SFRD) value of 0.0128 solar masses per year per cubic megaparsec is consistent with previous models for the SFRD derived using ultraviolet and infrared data. In Chapter 3, I present radio source counts across eight decades of flux density spanning 0.25 microJy < S < 25 Jy determined from the deepest 1.4 GHz radio continuum image taken by the MeerKAT radio interferometer in South Africa and the archival NVSS component catalog. With an rms noise of 0.56 microJy/beam and a resolution of 7.6’’, the MeerKAT DEEP2 image is confusion-limited, so below S=10 microJy I calculated the source counts statistically from the confusion brightness distribution P(D). Above S=10 microJy the source counts were measured directly from the DEEP2 image and the NVSS component catalog. The evolving energy-density function is the comoving energy density of radiation produced by sources at redshift z having spectral luminosity L_\nu at frequency \nu. Simple equations relate the brightness-weighted differential source counts S^2n(S) with the evolving energy-density function integrated over all redshifts (Appendix C). Using a combination of luminosity and density evolution, I developed evolutionary models (Chapter 4) for SFGs and AGNs that accurately predict the observed source counts given the local luminosity functions. Through the FIR/radio correlation, the product of luminosity and density evolution of radio sources is directly related to the total SFRD evolution, describing how many stars (by mass) were formed per year per comoving cubic megaparsec. The radio-derived model for SFRD evolution is similar to previous models based on UV/IR data, but predicts stronger star-formation evolution. Chapter 5 reviews the main conclusions of this dissertation and discusses future work.

Published
2021
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24. Forensic reconstruction of galaxy colour evolution and population characterisation

Author

Sabine Bellstedt, Jessica Thorne, Aaron Robotham, Matías Andrés Bravo Santa Cruz, Luke Davies, and Claudia Lagos

Subjects
ACTIVE GALACTIC NUCLEI, MAGNITUDE RELATION, SEMIANALYTIC MODEL, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, LUMINOSITY FUNCTIONS, Astrophysics - Astrophysics of Galaxies, QUENCHING TIME-SCALES, photometric [techniques], SPECTRAL-ENERGY-DISTRIBUTIONS, SUPERMASSIVE BLACK-HOLES, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MASS ASSEMBLY GAMA, Astrophysics::Solar and Stellar Astrophysics, STELLAR MASS, evolution [galaxies], Astrophysics::Galaxy Astrophysics, STAR-FORMATION HISTORIES
Abstract

Mapping the evolution of galaxy colours, from blue star-forming to red passive systems, is fundamental to understand the processes involved in galaxy evolution. To this end, we reconstruct the colour evolution of low-redshift galaxies, combining stellar templates with star formation and metallicity histories of galaxies from the Galaxy And Mass Assembly survey and \shark\ semi-analytic model. We use these colour histories to robustly characterise the evolution of red and blue galaxy populations over cosmic time. Using a Gaussian Mixture Model to characterise the colour distribution at any given epoch and stellar mass, we find both observations and simulations strongly favour a model with only two populations (blue and red), with no evidence for a third "green" population. We map the evolution of mean, weight, and scatter of the blue and red populations as a function of both stellar mass and lookback time. Using our simulated galaxy catalogue as a testbed, we find that we can accurately recover galaxies colour histories up to a lookback time of $\sim6$ Gyr. We find that both populations show little change in the mean colour for low-mass galaxies, while the colours at the massive end become significantly redder with time. The stellar mass above which the galaxy population is predominantly red decreases by 0.3 dex in the last 5 Gyrs. We find a good agreement between observations and simulations, with the largest tension being that massive galaxies from \shark\ are too blue (a known issue with many galaxy evolution models)., 23 pages, 16 figures. Accepted for publication in MNRAS

Published
2021
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25. On the accretion of a new group of galaxies onto Virgo: I. Internal kinematics of nine in-falling dEs

Author

Francesco La Barbera, Anna Pasquali, Thorsten Lisker, Rukmani Vijayaraghavan, Joachim Janz, Eric Emsellem, Bahar Bidaran, Glenn van de Ven, Jesús Falcón-Barroso, Agnieszka Sybilska, Dimitri A. Gadotti, Reynier Peletier, Lodovico Coccato, J. C. Gallagher, Eva K. Grebel, and Astronomy

Subjects
FOS: Physical sciences, DWARF ELLIPTIC GALAXIES, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, LUMINOSITY FUNCTIONS, 01 natural sciences, STAR-FORMATION, STELLAR POPULATIONS, Galaxy groups and clusters, Galaxy group, 0103 physical sciences, LINE KINEMATICS, galaxies: interactions, 010303 astronomy & astrophysics, Galaxy cluster, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, galaxies: dwarf, ATLAS(3D) PROJECT, SAURON PROJECT, Astrophysics - Astrophysics of Galaxies, Galaxy, Ram pressure, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MULTI-GAUSSIAN EXPANSION, galaxies: structure, DIGITAL SKY SURVEY, Halo, ANGULAR-MOMENTUM, galaxies: evolution
Abstract

Galaxy environment has been shown to play an important role in transforming late-type, star-forming galaxies to quiescent spheroids. This transformation is expected to be more severe for low-mass galaxies (M < $10^{10}$ \(M_\odot\)) in dense galaxy groups and clusters, mostly due to the influence of their past host halos (also known as pre-processing) and their present-day environments. For the first time, in this study, we investigate a sample of nine early-type dwarf galaxies (dEs) that were accreted as a likely bound group onto the Virgo galaxy cluster about 2-3 Gyr ago. Considering this special condition, these nine dEs may provide a test bed for distinguishing between the influence of the Virgo galaxy cluster and the effects of the previous host halo on their current properties. Specifically, we use VLT/MUSE integral-field unit spectra to derive their kinematics and specific angular momentum ($\lambda_{R}$) profiles. We observe a spread in the $\lambda_{R}$ profiles of our sample dEs, finding that the $\lambda_{R}$ profiles of half of them are as high as those of low-mass field galaxies. The remaining dEs exhibit $\lambda_{R}$ profiles as low as those of Virgo dEs that were likely accreted longer ago. Moreover, we detect nebular emission in one dE with a gas velocity offset suggesting ongoing gas stripping in Virgo. We suggest that the low-$\lambda_{R}$ dEs in our sample were processed by their previous host halo, prior to their infall to Virgo, and that the high-$\lambda_{R}$ dEs may be experiencing ram pressure stripping in Virgo., Comment: 23 pages, 16 figures, Accepted for publication in MNRAS

Published
2020

26. Galaxy And Mass Assembly (GAMA)

Author

Ivan K. Baldry, Jochen Liske, Andrew M. Hopkins, Sarah Brough, Helen M. Johnston, Michael Pracy, Benne W. Holwerda, Matt J. Jarvis, Scott M. Croom, Oliver Steele, Peder Norberg, Aaron S. G. Robotham, Matthew Colless, Lee S. Kelvin, Lingyu Wang, Daniel Thomas, Elaine M. Sadler, J. H. Y. Ching, Simon P. Driver, Jon Loveday, Joss Bland-Hawthorn, University of St Andrews. School of Physics and Astronomy, and Astronomy

Subjects
ACTIVE GALACTIC NUCLEI, Active galactic nucleus, Stellar mass, Radio galaxy, astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies [Radio continuum], Surveys, LUMINOSITY FUNCTIONS, 01 natural sciences, Luminosity, surveys, LOUD AGN, galaxies: groups: general, Galaxy group, 0103 physical sciences, QB Astronomy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, QB, STAR-FORMATION HISTORIES, Physics, radio continuum: galaxies, REDSHIFT SURVEY, INTERSTELLAR-MEDIUM, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, 3rd-DAS, Redshift survey, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, 1ST DATA RELEASE, HOST GALAXIES, groups: general [Galaxies], QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), DIGITAL SKY SURVEY, COOLING FLOWS
Abstract

We study the environments of low- and high- excitation radio galaxies (LERGs and HERGs respectively) in the redshift range $0.01 < z < 0.4$, using a sample of 399 radio galaxies and environmental measurements from the Galaxy And Mass Assembly (GAMA) survey. In our analysis we use the fifth nearest neighbour density ($\Sigma_{5}$) and the GAMA galaxy groups catalogue (G3Cv6) and construct control samples of galaxies matched in {\update stellar mass and colour} to the radio-detected sample. We find that LERGs and HERGs exist in different environments and that this difference is dependent on radio luminosity. High-luminosity LERGs ($L_{\rm NVSS} \gtrsim 10^{24}$ W Hz$^{-1}$) lie in much denser environments than a matched radio-quiet control sample (about three times as dense, as measured by $\Sigma_{5}$), and are more likely to be members of galaxy groups ($82^{+5}_{-7}$ percent of LERGs are in GAMA groups, compared to $58^{+3}_{-3}$ percent of the control sample). In contrast, the environments of the HERGs and lower luminosity LERGs are indistinguishable from that of a matched control sample. Our results imply that high-luminosity LERGs lie in more massive haloes than non-radio galaxies of similar stellar mass and colour, in agreement with earlier studies (Wake et al. 2008; Donoso et al. 2010). When we control for the preference of LERGs to be found in groups, both high- and low- luminosity LERGs are found in higher-mass haloes ($\sim 0.2$ dex; at least 97 percent significant) than the non-radio control sample., Comment: 18 pages, 11 figures. Accepted for publication by MNRAS

Published
2017
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27. Luminosity functions and star formation rates at z ∼6–10: Galaxy buildup in the reionization age

Author

Bouwens, Rychard and Illingworth, Garth

Subjects
*GALAXIES, *ASTRONOMY, *METAPHYSICAL cosmology, *STELLAR luminosity function, *STELLAR magnitudes
Abstract

Abstract: HST ACS and NICMOS data are now of sufficient depth and areal coverage to place strong constraints on the formation and evolution of galaxies during the first 1–2Gyrs of the universe. Of particular interest are galaxies at z ∼6 since they represent the earliest epoch accessible to current high-efficiency optical instrumentation. To this end, we have been involved in the systematic construction of a large sample of 346 z ∼6 objects from all the deepest wide-area HST data (UDF, UDF-Parallel, and GOODS fields). They have been used to construct an optimal determination of the rest-frame continuum UV LF at z ∼6. Our LF extends to over 3 magnitudes below L*, fainter than has been done at z ∼3. Over the interval z ∼6 to z ∼3, we find strong evidence for evolution in the UV LF. Though we can thus far make no strong claims on an evolution of the faint end slope, the characteristic luminosity appears to have approximately doubled over the interval z ∼6 to z ∼3, consistent with hierarchical expectations. Remarkably, this shift to lower luminosities extends to even higher redshifts. Using all deep J + H NICMOS observations (800 orbits in total), we have been able to demonstrate that the bright end of the LF is at least 5 times lower at z ∼10 than at z ∼4, with a similar deficit being established from our recent detections and first statistical sample of z ∼7–8 galaxies using our UDF NICMOS data. In these precedings, we discuss what is known about the UV LF and UV luminosity density at z ∼6–10 from current data and its evolution relative to z ∼3. We also describe several exciting prospects for advance in this area over the next year. [Copyright &y& Elsevier]

Published
2006
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28. The Luminosity Function of Low-Mass X-ray Binaries in Galaxies.

Author

Postnov, K.A. and Kuranov, A.G.

Subjects
*GALAXIES, *X-ray binaries, *BINARY stars, *X-ray astronomy, *MASS transfer, *ASTRONOMY
Abstract

The X-ray luminosity function of low-mass binaries constructed from the observations of pointlike X-ray sources in galactic bulges can be explained in terms of the main evolutionary relations for the rate of mass transfer onto a compact object. The observed scatter of luminosities for individual low-mass X-ray sources in our Galaxy is shown to be satisfactorily described by a symmetric quasi-Lorentz curve with a dispersion proportional to the mean luminosity. Such a form of the mean luminosity function for individual sources does riot affect the power-law pattern of the luminosity function for the entire population of sources that is expected for a power-law dependence of the mass transfer rate in a close binary on the mass of the Roche lobe-filling optical component. [ABSTRACT FROM AUTHOR]

Published
2005
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29. A significant excess in major merger rate for AGNs with the highest eddington ratios at z < 0.2

Author

Bernd Husemann, John D. Silverman, Arjen van der Wel, M. Mechtley, Rogier A. Windhorst, Andreas Schulze, I. Smirnova-Pinchukova, M. Schramm, Victor Marian, Eduardo Bañados, Anton M. Koekemoer, Jan Torge Schindler, Irham Taufik Andika, Seth H. Cohen, Melanie Kaasinen, Masafusa Onoue, Knud Jahnke, Carolin Villforth, and Vardha N. Bennert

Subjects
Active galactic nucleus, STELLAR MASSES, Galaxy mergers, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy merger, STAR-FORMATION RATES, LUMINOSITY FUNCTIONS, SUPERMASSIVE BLACK-HOLES, ELLIPTIC GALAXIES, Galaxy evolution, Supermassive black holes, Galaxy formation and evolution, Quasars, Astrophysics::Galaxy Astrophysics, AGN host galaxies, Physics, Supermassive black hole, Active galactic nuclei, Quasar, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, EVOLUTION, HOST GALAXY MORPHOLOGIES, Physics and Astronomy, COSMOLOGICAL SIMULATIONS, Space and Planetary Science, BULGE MASS, BORDA COUNT
Abstract

Observational studies are increasingly finding evidence against major mergers being the dominant mechanism responsible for triggering AGN. After studying the connection between major mergers and AGN with the highest Eddington ratios at z=2, we here expand our analysis to z0.3, and 25 mass- and redshift-matched control galaxies. To match the appearance of the two samples, we add synthetic point sources to the inactive comparison galaxies. The combined sample of AGN and inactive galaxies was independently ranked by 19 experts with respect to the degree of morphological distortion. We combine the resulting individual rankings into multiple overall rankings, from which we derive the respective major merger fractions of the two samples. With a best estimate of 0.41 $\pm$ 0.12 for the AGN host galaxies and 0.08 $\pm$ 0.06 for the inactive galaxies our results imply that our AGN host galaxies have a significantly higher merger rate, regardless of the observed wavelength or applied methodology. We conclude that although major mergers are an essential mechanism to trigger local high Eddington ratio AGNs at z=50% of this specific AGN subpopulation still remains unclear., Comment: 17 pages (plus 23 pages appendix), 8 figures, 3 tables; Accepted for publication in ApJ

Published
2020

30. Evolution of the cold gas properties of simulated post-starburst galaxies

Author

Kate Rowlands, Timothy A. Davis, Stuart McAlpine, Freeke van de Voort, Vivienne Wild, Robert A. Crain, Department of Physics, University of Helsinki, Department of Physics, and University of St Andrews. School of Physics and Astronomy

Subjects
galaxies: starburst, interactions [Galaxies], Astrophysics, ATOMIC-HYDROGEN, 01 natural sciences, galaxies: interactions, QB Astronomy, 010303 astronomy & astrophysics, QC, galaxies: kinematics and dynamics, QB, STAR-FORMATION HISTORIES, Physics, E PLUS, REDSHIFT SURVEY, education.field_of_study, kinematics and dynamics [Galaxies], 3rd-DAS, Redshift survey, MOLECULAR GAS, STELLAR POPULATION SYNTHESIS, EAGLE SIMULATIONS, galaxies: evolution, galaxies: ISM, Active galactic nucleus, Stellar mass, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, LUMINOSITY FUNCTIONS, star formation [Galaxies], ISM [Galaxies], 0103 physical sciences, education, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Star formation, Time evolution, Astronomy and Astrophysics, evolution [Galaxies], ATLAS(3D) PROJECT, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, starburst [Galaxies], QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, FORMATION LAWS, sense organs
Abstract

Post-starburst galaxies are typically considered to be a transition population, en route to the red sequence after a recent quenching event. Despite this, recent observations have shown that these objects typically have large reservoirs of cold molecular gas. In this paper we study the star-forming gas properties of a large sample of post-starburst galaxies selected from the cosmological, hydrodynamical EAGLE simulations. These objects resemble observed high-mass post-starburst galaxies both spectroscopically and in terms of their space density, stellar mass distribution and sizes. We find that the vast majority of simulated post-starburst galaxies have significant gas reservoirs, with star-forming gas masses of ~10$^9$ M$_{\odot}$, in good agreement with those seen in observational samples. The simulation reproduces the observed time evolution of the gas fraction of the post-starburst galaxy population, with the average galaxy losing ~90 per cent of its star-forming interstellar medium in only ~600 Myr. A variety of gas consumption/loss processes are responsible for this rapid evolution, including mergers and environmental effects, while active galactic nuclei play only a secondary role. The fast evolution in the gas fraction of post-starburst galaxies is accompanied by a clear decrease in the efficiency of star formation, due to a decrease in the dense gas fraction. We predict that forthcoming ALMA observations of the gas reservoirs of low-redshift post-starburst galaxies will show that the molecular gas is typically compact and has disturbed kinematics, reflecting the disruptive nature of many of the evolutionary pathways that build up the post-starburst galaxy population., 15 pages, 17 figures, MNRAS accepted

Published
2018

31. A Foreground Masking Strategy for [C II] Intensity Mapping Experiments Using Galaxies Selected by Stellar Mass and Redshift

Author

Jonathon Hunacek, Guochao Sun, Bade Uzgil, Marta B. Silva, Asantha Cooray, Marco P. Viero, Tzu-Ching Chang, C. Matt Bradford, A. T. Crites, Lorenzo Moncelsi, Yun-Ting Cheng, Steve Hailey-Dunsheath, James J. Bock, Michael Zemcov, and Astronomy

Subjects
Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, first stars, MU-M, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, LUMINOSITY FUNCTIONS, STAR-FORMATION-RATE, 01 natural sciences, ALMA SPECTROSCOPIC SURVEY, 0103 physical sciences, dark ages, reionization, first stars, Emission spectrum, dark ages, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Line (formation), large-scale structure of universe, LEGACY SURVEY, Physics, 010308 nuclear & particles physics, REIONIZATION, Intensity mapping, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, MOLECULAR GAS, EVOLUTION, Galaxy, Redshift, diffuse radiation, COSMOS FIELD, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, EAGLE SIMULATIONS, intergalactic medium, Intensity (heat transfer)
Abstract

Intensity mapping provides a unique means to probe the epoch of reionization (EoR), when the neutral intergalactic medium was ionized by the energetic photons emitted from the first galaxies. The [CII] 158$��$m fine-structure line is typically one of the brightest emission lines of star-forming galaxies and thus a promising tracer of the global EoR star-formation activity. However, [CII] intensity maps at $6 \lesssim z \lesssim 8$ are contaminated by interloping CO rotational line emission ($3 \leq J_{\rm upp} \leq 6$) from lower-redshift galaxies. Here we present a strategy to remove the foreground contamination in upcoming [CII] intensity mapping experiments, guided by a model of CO emission from foreground galaxies. The model is based on empirical measurements of the mean and scatter of the total infrared luminosities of galaxies at $z < 3$ and with stellar masses $M_{*} > 10^{8}\,\rm M_{\rm \odot}$ selected in $K$-band from the COSMOS/UltraVISTA survey, which can be converted to CO line strengths. For a mock field of the Tomographic Ionized-carbon Mapping Experiment (TIME), we find that masking out the "voxels" (spectral-spatial elements) containing foreground galaxies identified using an optimized CO flux threshold results in a $z$-dependent criterion $m^{\rm AB}_{\rm K} \lesssim 22$ (or $M_{*} \gtrsim 10^{9} \,\rm M_{\rm \odot}$) at $z < 1$ and makes a [CII]/CO$_{\rm tot}$ power ratio of $\gtrsim 10$ at $k=0.1$ $h$/Mpc achievable, at the cost of a moderate $\lesssim 8\%$ loss of total survey volume., 14 figures, 4 tables, re-submitted to ApJ after addressing reviewer's comments. Comments welcome

Published
2018

32. The new galaxy evolution paradigm revealed by the Herschel surveys

Author

Matt J. Jarvis, Daniel J. Smith, Lucia Marchetti, Aaron S. G. Robotham, C. Furlanetto, Jon Loveday, Nathan Bourne, Gianfranco De Zotti, Simon Dye, Stephen Anthony Eales, Loretta Dunne, Kate Rowlands, Paul van der Werf, A. H. Wright, Rob Ivison, Catherine Vlahakis, S. Phillipps, Elisabetta Valiante, Sebastian Viaene, Simon P. Driver, Michał J. Michałowski, Edward N. Taylor, Matthew Smith, Philip Cigan, Steve Maddox, and University of St Andrews. School of Physics and Astronomy

Subjects
INITIAL MASS FUNCTION, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, LUMINOSITY FUNCTIONS, SCALING RELATIONS, 01 natural sciences, Peculiar galaxy, Galaxy group, 0103 physical sciences, STAR-FORMING GALAXIES, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, NEARBY GALAXIES, Interacting galaxy, Brightest cluster galaxy, 010303 astronomy & astrophysics, Lenticular galaxy, QC, Astrophysics::Galaxy Astrophysics, QB, Dwarf galaxy, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, 3rd-DAS, DISK GALAXIES, ATLAS(3D) PROJECT, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, MOLECULAR GAS, SUBMILLIMETER WAVELENGTHS, QC Physics, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Elliptical galaxy, DIGITAL SKY SURVEY, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution
Abstract

The Herschel Space Observatory has revealed a very different galaxyscape from that shown by optical surveys which presents a challenge for galaxy-evolution models. The Herschel surveys reveal (1) that there was rapid galaxy evolution in the very recent past and (2) that galaxies lie on a a single Galaxy Sequence (GS) rather than a star-forming `main sequence' and a separate region of `passive' or `red-and-dead' galaxies. The form of the GS is now clearer because far-infrared surveys such as the Herschel ATLAS pick up a population of optically-red star-forming galaxies that would have been classified as passive using most optical criteria. The space-density of this population is at least as high as the traditional star-forming population. By stacking spectra of H-ATLAS galaxies over the redshift range 0.001 < z < 0.4, we show that the galaxies responsible for the rapid low-redshift evolution have high stellar masses, high star-formation rates but, even several billion years in the past, old stellar populations - they are thus likely to be relatively recent ancestors of early-type galaxies in the Universe today. The form of the GS is inconsistent with rapid quenching models and neither the analytic bathtub model nor the hydrodynamical EAGLE simulation can reproduce the rapid cosmic evolution. We propose a new gentler model of galaxy evolution that can explain the new Herschel results and other key properties of the galaxy population., Accepted for publication in MNRAS

Published
2018
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33. Synchrotron emission of galaxies

Author

Šlaus, Bruno and Smolčić, Vernesa

Subjects
PRIRODNE ZNANOSTI. Fizika, funkcije luminoziteta, synchrotron radiation, aktivne galaktičke jezgre, active galactic nuclei, radio observations, spektralni indeksi, spectral index, sinkrotronsko zračenje, radio opažanja, luminosity functions, NATURAL SCIENCES. Physics
Abstract

Sinkrotronsko zračenje, koje nastaje interakcijom magnetskog polja i relativistički ubrzanih nabijenih čestica, dominantan je oblik zračenja galaksija u radio području. Sinkrotronsko zračenje javlja se pri prirastu (akreciji) materijala na središnju supermasivnu crnu rupu. Opažanja u radio području stoga su neizostavan dio proučavanja aktivnih galaktičkih jezgri. U ovom radu se promatra radio emisija na frekvenciji 610 MHz unutar XXL-North polja. Koristimo podatke koji dolaze od opažanja Giant Metrewave Radio Telescope (GMRT) radio teleskopom. Radi detekcijskog limita istraživanja uzorak opaženih izvora sastoji se uglavnom od aktivnih galaktičkih jezgri. Podatke korigiramo eliminacijom efekta kromatske aberacije, odvajamo razlućene od nerazlučenih izvora, te izdvajamo sve izvore koji se sastoje od više komponenti. Koristeći podatke The NRAO VLA Sky Survey (NVSS) istraživanja na 1400 MHz računamo spektralne indekse detektiranih izvora, koji su izravno povezani s oblikom energetske raspodjele čestica odgovornih za opaženo sinkrotronsko zračenje. Uočavamo razlike između spektralnih indeksa razlučenih i nerazlučenih izvora koje pripisujemo razlikama u prirodi samih emitera. Činjenicu da nerazlučeni izvori u prosjeku posjeduju veći broj ravnih spektara objašnjavamo time da je emisija nerazlučenih izvora u pravilu dominirana zračenjem iz njihove optički duboke sredine, dok razlučeni izvori zrače iz svojih optički tankih radio izbočina (proširenog završetka radio mlazova prisutnoga kod radio glasnih aktivnih galaktičkih jezgri). Koristeći fotometrijski određene crvene pomake, konstruiramo funkcije luminoziteta promatranoga uzorka. Pritom uzorak razdvajamo na više podskupova ograničenih crvenih pomaka radi postojanja evolucije funkcija luminoziteta. Usporedujemo stvorene funkcije luminoziteta s podacima ostalih istraživanja te s modelom evolucije preuzetim iz literature. Zaključujemo da su slaganja dobra. Važnost naših podataka leži u tome da se, radi širine i relativne dubine polja, nalaze u sredini između istraživanja velike dubine preko malenoga nebeskog polja i plićih istraživanja preko velikih nebeskih površina. Synchrotron emission arising from the accelerated motion of charged particles is the dominant form of radio emission from galaxies. It is observed in the process of accretion of material into the central supermassive black hole. Observations in the radio part of the spectrum are important for understanding the nature of active galactic nuclei. Our observations are carried out at the frequency of 610 MHz inside the XXL-North field, with the Giant Metrewave Radio Telescope (GMRT). Because of the detection limit of our observations, the majority of our sample consists of active galactic nuclei. We eliminate effects of bandwidth smearing, separate resolved from unresolved sources and classify the multi-component sources. Using The NRAO VLA Sky Survey (NVSS) data at 1400 MHz we calculate the spectral indices of our sources, which are directly connected to the shape of the energy distribution of the emitting particles. The spectral indices of resolved and unresolved sources differ slightly, which we explain by the difference in the nature of these emitters. The unresolved sources emit radiation mostly from the core which is optically thick, while the resolved sources emit radiation from the optically thin radio lobes. By using the photometrically derived redshifts, we were able to construct the luminosity functions of our sample. To assess the evolution of the luminosity functions we separate our data into redshift subsets. We compare our luminosity functions with values from other surveys and with a model of luminosity function evolution taken from literature. The importance of our observations lays in the mixture of depth and width of our survey, which provides a bridge between the very deep surveys directed towards small areas of the sky and the very wide but shallow surveys.

Published
2018

34. Herschel *-ATLAS: deep HST/WFC3 imaging of strongly lensed submillimetre galaxies

Author

William J. Sutherland, Loretta Dunne, Michael Pohlen, D. J. B. Smith, Edo Ibar, A. Dariush, R. Hopwood, Antonio Cava, Pasquale Temi, E. da Cunha, Stephen Anthony Eales, Simon Dye, Lerothodi Leonard Leeuw, Jacopo Fritz, G. de Zotti, Helmut Dannerbauer, Asantha Cooray, S. Buttiglione, Michał J. Michałowski, S. Fleuren, J. González-Nuevo, Kate Rowlands, S. Kim, Julie Wardlow, Alain Omont, R. S. Bussmann, Stephen Serjeant, Robbie Richard Auld, Luigi Danese, Maarten Baes, E. E. Rigby, Enzo Pascale, Steve Maddox, Andrea Lapi, S. Amber, Rob Ivison, Mattia Negrello, Marcella Massardi, Istituto Nazionale di Astrofisica, Agenzia Spaziale Italiana, Science and Technology Facilities Council (UK), Ministerio de Ciencia e Innovación (España), Consejo Superior de Investigaciones Científicas (España), European Commission, University of St Andrews. School of Physics and Astronomy, and Universidad de Cantabria

Subjects
Gravitational lensing: strong, DUST, Astrophysics, Galaxies: formation, galaxies [infrared], 01 natural sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QC, QB, Physics, COSMIC cancer database, Galaxies: evolution, Galaxies: elliptical and lenticular, cD, strong [gravitational lensing], Elliptical galaxy, Astrophysics::Earth and Planetary Astrophysics, formation [galaxies], INFRARED-EMISSION, Astrophysics::Cosmology and Extragalactic Astrophysics, elliptical and lenticular, cD [Galaxies], LUMINOSITY FUNCTIONS, cD, Submillimetre: galaxies, Settore FIS/05 - Astronomia e Astrofisica, EXTRAGALACTIC SURVEY, galaxies [submillimetre], 0103 physical sciences, SIMPLE-MODEL, BLACK-HOLES, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Luminous infrared galaxy, Galaxies: elliptical and lenticular, 010308 nuclear & particles physics, Star formation, Astronomy, Astronomy and Astrophysics, Infrared: galaxies, Space and Planetary Science, EVOLUTION, Galaxy, Stars, Photometry (astronomy), QC Physics, STELLAR, Gravitational lens, Physics and Astronomy, gravitational lensing: strong, galaxies: elliptical and lenticular, cD, galaxies: evolution, galaxies: formation, infrared: galaxies, submillimetre: galaxies, HIGH-REDSHIFT, SCIENCE DEMONSTRATION PHASE, elliptical and lenticular [galaxies]
Abstract

M. Negrello et al., We report on deep near-infrared observations obtained with the Wide Field Camera-3 (WFC3) onboard the Hubble Space Telescope (HST) of the first five confirmed gravitational lensing events discovered by the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). We succeed in disentangling the background galaxy from the lens to gain separate photometry of the two components. The HST data allow us to significantly improve on previous constraints of the mass in stars of the lensed galaxy and to perform accurate lens modelling of these systems, as described in the accompanying paper by Dye et al. We fit the spectral energy distributions of the background sources from near-IR to millimetre wavelengths and use the magnification factors estimated by Dye et al. to derive the intrinsic properties of the lensed galaxies. We find these galaxies to have star-formations rates (SFR) ~ 400-2000 M⊙ yr-1, with ~(6-25) × 1010 M⊙ of their baryonic mass already turned into stars. At these rates of star formation, all remaining molecular gas will be exhausted in less than ~100 Myr, reaching a final mass in stars of a few 1011 M⊙. These galaxies are thus proto-ellipticals caught during their major episode of star formation, and observed at the peak epoch (z ~ 1.5-3) of the cosmic star formation history of the Universe., This work was supported by STFC (grants PP/D002400/1 and ST/G002533/1), by ASI/INAF agreement I/072/09/0, by PRININAF 2012 project ‘Looking into the dust-obscured phase of galaxy formation through cosmic zoom lenses in the Herschel Astrophysical Large Area Survey’ and, in part, by the Spanish Ministerio de Ciencia e Innovacion (project AYA2010-21766-C03-01). JGN acknowledges financial support from the Spanish CSIC for a JAE-DOC fellowship, co-funded by the European Social Fund.

Published
2014
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35. MUSE deep-fields: the Ly alpha luminosity function in the Hubble Deep Field-South at 2.91 < z < 6.64

Author

Drake, A.B., Guiderdoni, B., Blaizot, J., Wisotzki, L., Herenz, E.C., Garel, T., Richard, J., Bacon, R., Bina, D., Cantalupo, S., Contini, T., Brok, M., Hashimoto, T., Marino, R.A., Pelló, R., Schaye, J., and Schmidt, K.B.

Subjects
galaxies: luminosity functions, surveys, galaxies: high-redshift, luminosity functions, mass function, cosmology: observations, galaxies: evolution, galaxies: formation, galaxies: high-redshift [galaxies]
Abstract

We present the first estimate of the Ly α luminosity function using blind spectroscopy from the Multi Unit Spectroscopic Explorer, MUSE, in the Hubble Deep Field-South. Using automatic source-detection software, we assemble a homogeneously detected sample of 59 Ly α emitters covering a flux range of −18.0 < log10 (F) < −16.3 (erg s−1 cm−2), corresponding to luminosities of 41.4 < log10 (L) < 42.8 (erg s−1). As recent studies have shown, Ly α fluxes can be underestimated by a factor of 2 or more via traditional methods, and so we undertake a careful assessment of each object's Ly α flux using a curve-of-growth analysis to account for extended emission. We describe our self-consistent method for determining the completeness of the sample, and present an estimate of the global Ly α luminosity function between redshifts 2.91 < z < 6.64 using the 1/Vmax estimator. We find that the luminosity function is higher than many number densities reported in the literature by a factor of 2–3, although our result is consistent at the 1σ level with most of these studies. Our observed luminosity function is also in good agreement with predictions from semi-analytic models, and shows no evidence for strong evolution between the high- and low-redshift halves of the data. We demonstrate that one's approach to Ly α flux estimation does alter the observed luminosity function, and caution that accurate flux assessments will be crucial in measurements of the faint-end slope. This is a pilot study for the Ly α luminosity function in the MUSE deep-fields, to be built on with data from the Hubble Ultra Deep Field that will increase the size of our sample by almost a factor of 10., Monthly Notices of the Royal Astronomical Society, 471 (1), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711

Published
2017

36. Herschel star-ATLAS/GAMA: the environmental density of far-infrared bright galaxies at z < 0.5

Author

R. Hopwood, Aliakbar Dariush, Daniel J. Smith, Martin J. Hardcastle, Elisabetta Valiante, Nathan Bourne, Maarten Baes, Edo Ibar, C. S. Burton, Jonathan Loveday, Jochen Liske, G. de Zotti, Matthew Smith, Mattia Negrello, Stephen Anthony Eales, Rob Ivison, Steve Maddox, Jamie Stevens, Asantha Cooray, Loretta Dunne, Antonio Cava, David Bonfield, Matt J. Jarvis, and Sarah Brough

Subjects
ACTIVE GALACTIC NUCLEI, statistics [galaxies], Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, formation [galaxies], EARLY DATA RELEASE, statistical [methods], FOS: Physical sciences, Astrophysics, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, LUMINOSITY FUNCTIONS, galaxies [infrared], Luminosity, VORONOI TESSELLATIONS, evolution [galaxies], Astrophysics::Galaxy Astrophysics, QB, Physics, Luminous infrared galaxy, Star formation, Astronomy, Astronomy and Astrophysics, Redshift survey, Galaxy, Redshift, FORMATION RATES, Physics and Astronomy, Space and Planetary Science, MASS ASSEMBLY GAMA, DIGITAL SKY SURVEY, Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], STELLAR MASS, SCIENCE DEMONSTRATION PHASE, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We compare the environmental and star formation properties of far-infrared detected and non--far-infrared detected galaxies out to $z \sim0.5$. Using optical spectroscopy and photometry from the Galaxy And Mass Assembly (GAMA) and Sloan Digital Sky Survey (SDSS), with far-infrared observations from the {\em Herschel}-ATLAS Science Demonstration Phase (SDP), we apply the technique of Voronoi Tessellations to analyse the environmental densities of individual galaxies. Applying statistical analyses to colour, $r-$band magnitude and redshift-matched samples, we show there to be a significant difference at the 3.5$\sigma$ level between the normalized environmental densities of these two populations. This is such that infrared emission (a tracer of star formation activity) favours underdense regions compared to those inhabited by exclusively optically observed galaxies selected to be of the same $r-$band magnitude, colour and redshift. Thus more highly star-forming galaxies are found to reside in the most underdense environments, confirming previous studies that have proposed such a correlation. However, the degeneracy between redshift and far-infrared luminosity in our flux-density limited sample means that we are unable to make a stronger statement in this respect. We then apply our method to synthetic light cones generated from semi-analytic models, finding that over the whole redshift distribution the same correlations between star-formation rate and environmental density are found., Comment: 16 pages, 12 figures, 10 tables

Published
2016

37. Understanding the H2/HI Ratio in Galaxies

Author

Steve Rawlings and Danail Obreschkow

Subjects
Molecular Gas, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ISM: atoms, Elliptic Galaxies, Conversion Factor, Omega, ISM: clouds, Luminosity Functions, Phenomenological model, Interstellar-Medium, Hipass Catalog, Astrophysics::Galaxy Astrophysics, media_common, Physics, radio lines: galaxies, Spiral galaxy, Spiral Galaxies, Gamma-Ray Emission, HIPASS, Lyman-Alpha Systems, Astronomy and Astrophysics, Star-Formation, Mass ratio, Astrophysics - Astrophysics of Galaxies, Galaxy, Universe, Redshift, ISM: molecules, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract

We revisit the mass ratio Rmol between molecular hydrogen (H2) and atomic hydrogen (HI) in different galaxies from a phenomenological and theoretical viewpoint. First, the local H2-mass function (MF) is estimated from the local CO-luminosity function (LF) of the FCRAO Extragalactic CO-Survey, adopting a variable CO-to-H2 conversion fitted to nearby observations. This implies an average H2-density Omega_H2=(6.9+-2.7) 10^5/h and Omega_H2/Omega_HI=0.26+-0.11 in the local Universe. Second, we investigate the correlations between Rmol and global galaxy properties in a sample of 245 local galaxies. Based on these correlations we introduce four phenomenological models for Rmol, which we apply to estimate H2-masses for each HI-galaxy in the HIPASS catalogue. The resulting H2-MFs (one for each model for Rmol) are compared to the reference H2-MF derived from the CO-LF, thus allowing us to determine the Bayesian evidence of each model and to identify a clear best model, in which, for spiral galaxies, Rmol negatively correlates with both galaxy Hubble type and total gas mass. Third, we derive a theoretical model for Rmol for regular galaxies based on an expression for their axially symmetric pressure profile dictating the degree of molecularization. This model is quantitatively similar to the best phenomenological one at redshift z=0, and hence represents a consistent generalization while providing a physical explanation for the dependence of Rmol on global galaxy properties. Applying the best phenomenological model for Rmol to the HIPASS sample, we derive the first integral cold gas-MF (HI+H2+helium) of the local Universe., Comment: 20 pages, 13 figures, 6 tables

Published
2016

38. Cosmology with intensity mapping techniques using atomic and molecular lines

Author

Mario G. Santos, Asantha Cooray, Marta B. Silva, José Fonseca, and Astronomy

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), EMITTING GALAXIES, Infrared, REDSHIFT, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, LUMINOSITY FUNCTIONS, 01 natural sciences, Cosmology, law.invention, Telescope, LY-ALPHA, law, C II, 0103 physical sciences, STAR-FORMING GALAXIES, Emission spectrum, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, REIONIZATION, Intensity mapping, Astronomy, Astronomy and Astrophysics, H I, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, LYMAN-CONTINUUM EMISSION, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), ALPHA ESCAPE FRACTION, large-scale structure of Universe, cosmology: miscellaneous, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a systematic study of the intensity mapping technique using updated models for the different emission lines from galaxies and identify which ones are more promising for cosmological studies of the post reionization epoch. We consider the emission of ${\rm Ly\alpha}$, ${\rm H\alpha}$, H$\beta$, optical and infrared oxygen lines, nitrogen lines, CII and the CO rotational lines. We then identify that ${\rm Ly\alpha}$, ${\rm H\alpha}$, OII, CII and the lowest rotational CO lines are the best candidates to be used as IM probes. These lines form a complementary set of probes of the galaxies emission spectra. We then use reasonable experimental setups from current, planned or proposed experiments to access the detectability of the power spectrum of each emission line. Intensity mapping of ${\rm Ly\alpha}$ emission from $z=2$ to 3 will be possible in the near future with HETDEX, while far-infrared lines require new dedicated experiments. We also show that the proposed SPHEREx satellite can use OII and ${\rm H\alpha}$ IM to study the large-scale distribution of matter in intermediate redshifts of 1 to 4. We found that submilimeter experiments with bolometers can have similar performances at intermediate redshifts using CII and CO(3-2)., Comment: 18 pages, 21 figures, 5 tables, published in MNRAS, typos corrected

Published
2016

39. Gran Telescopio Canarias observations of an overdense region of Lyman alpha emitters at z=6.5

Author

Gallego Maestro, Jesús, otros, ..., Gallego Maestro, Jesús, and otros, ...

Abstract

© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Artículo firmado por 15 autores. This work is based on observations made during observing semesters 2011B and 2012B at GTC, which is located at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma, Spain. The observation time allocated was 14 h via the University of Florida and 20.33 h via collaborators in Spain and México. We are thankful for help and support during the observation runs from Antonio Cabrera Lavers and GTC staff. This work is (partly) based on data obtained with the SHARDS filter set, purchased by Universidad Complutense de Madrid (UCM). SHARDS was funded by the Spanish Government through grant AYA2012-31277.; Furthermore, this research made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.; We are thankful for the funding support provided to the graduate student working on this project through a Royal Thai Government Scholarship from the National Astronomical Research Institute of Thailand (NARIT). JMRE, RC and NCR (AYA2012-39168-C03-01), ESS and AM (AYA2012-39168-C03-02), and JMMH (AYA2010-21887-C04-04, AYA2010-21887-C04-02 and AYA2012-39362-C02-01) acknowledge support from the Spanish MINECO under the PNAyA grants given in parenthesis. ET, RT and IA acknowledge support from the Mexican Research Council (CONACYT) under grants 2008-103365, 2010-01-155046 and 2011-01-167291., We present the results of our search near the end of the Reionization Epoch for faint galaxies. This has been done using very deep OSIRIS images obtained at the Gran Telescopio Canarias (GTC). Our observations focus around two close, massive Lyman alpha emitters (LAEs) at redshift 6.5, discovered in the SXDS field within a large-scale overdense region. The total GTC observing time in three medium band filters (F883w35, F913w25 and F941w33) is over 34 h covering 7.0 x 8.5 arcmin(2) (or similar to 30 000 Mpc(3) at z = 6.5). In addition to the two spectroscopically confirmed LAEs in the field, we have identified 45 other LAE candidates. The preliminary luminosity function derived from our observations, assuming a spectroscopic confirmation success rate of 2/3 as in previous surveys, suggests this area is about 2 times denser than the general field galaxy population at z = 6.5. If confirmed spectroscopically, our results will imply the discovery of one of the earliest protoclusters in the Universe, which will evolve to resemble the most massive galaxy clusters today., Ministerio de Economía y Competitividad (MINECO), National Aeronautics and Space Administration, National Astronomical Research Institute of Thailand (NARIT), Mexican Research Council (CONACYT), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2017

40. The Ages of the Thin Disk, Thick Disk, and the Halo from Nearby White Dwarfs

Author

1777676, Kilic, Mukremin, von Hippel, Ted, Munn, Jeffrey A., Harris, Hugh C., Liebert, James W., et al., 1777676, Kilic, Mukremin, von Hippel, Ted, Munn, Jeffrey A., Harris, Hugh C., Liebert, James W., and et al.

Abstract

We present a detailed analysis of the white dwarf luminosity functions derived from the local 40 pc sample and the deep proper motion catalog of Munn et al. (2014, 2017). Many of the previous studies ignored the contribution of thick disk white dwarfs to the Galactic disk luminosity function, which results in an erronous age measurement. We demonstrate that the ratio of thick/thin disk white dwarfs is roughly 20% in the local sample. Simultaneously fitting for both disk components, we derive ages of 6.8-7.0 Gyr for the thin disk and 8.7 ± 0.1 Gyr for the thick disk from the local 40 pc sample. Similarly, we derive ages of 7.4-8.2 Gyr for the thin disk and 9.5-9.9 Gyr for the thick disk from the deep proper motion catalog, which shows no evidence of a deviation from a constant star formation rate in the past 2.5 Gyr. We constrain the time difference between the onset of star formation in the thin disk and the thick disk to be 1.6 +0.3−0.4 Gyr. The faint end of the luminosity function for the halo white dwarfs is less constrained, resulting in an age estimate of 12.5 +1.4−3.4 Gyr for the Galactic inner halo. This is the first time ages for all three major components of the Galaxy are obtained from a sample of field white dwarfs that is large enough to contain significant numbers of disk and halo objects. The resultant ages agree reasonably well with the age estimates for the oldest open and globular clusters.

Published
2017

41. SIMULATION OF THE COSMIC EVOLUTION OF ATOMIC AND MOLECULAR HYDROGEN IN GALAXIES

Author

Sadegh Khochfar, Danail Obreschkow, Steve Rawlings, G. De Lucia, and Darren J. Croton

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Hydrogen, media_common.quotation_subject, FOS: Physical sciences, chemistry.chemical_element, Tully-Fisher Relation, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, ISM: atoms, Star-Forming Galaxies, ISM: clouds, Integral Field Spectroscopy, Physical cosmology, Large-Scale Structure, Luminosity Functions, Emission spectrum, On Spiral Galaxies, Astrophysics::Galaxy Astrophysics, Helium, media_common, radio lines: galaxies, Physics, Nearby Galaxies, COSMIC cancer database, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, ISM: molecules, Universe, Galaxy, Redshift, chemistry, Uv-Selected Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Redshift Survey, Astrophysics - Cosmology and Nongalactic Astrophysics, H-I
Abstract

We present a simulation of the cosmic evolution of the atomic and molecular phases of the cold hydrogen gas in about 3e7 galaxies, obtained by post-processing the virtual galaxy catalog produced by (De Lucia et al. 2007) on the Millennium Simulation of cosmic structure (Springel et al. 2005). Our method uses a set of physical prescriptions to assign neutral atomic hydrogen (HI) and molecular hydrogen (H2) to galaxies, based on their total cold gas masses and a few additional galaxy properties. These prescriptions are specially designed for large cosmological simulations, where, given current computational limitations, individual galaxies can only be represented by simplistic model-objects with a few global properties. Our recipes allow us to (i) split total cold gas masses between HI, H2, and Helium, (ii) assign realistic sizes to both the HI- and H2-disks, and (iii) evaluate the corresponding velocity profiles and shapes of the characteristic radio emission lines. The results presented in this paper include the local HI- and H2-mass functions, the CO-luminosity function, the cold gas mass--diameter relation, and the Tully-Fisher relation (TFR), which all match recent observational data from the local Universe. We also present high-redshift predictions of cold gas diameters and the TFR, both of which appear to evolve markedly with redshift., 19 pages, 15 figures

Published
2009
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42. Radiation from early black holes - I. Effects on the neutral intergalactic medium

Author

Michela Mapelli, E. Ripamonti, Saleem Zaroubi, Astronomy, University of Zurich, and Ripamonti, E

Subjects
ACTIVE GALACTIC NUCLEI, Black hole physics, Cosmology: theory, Diffuse radiation, Galaxies: formation, Intergalactic medium, Astronomy and Astrophysics, Space and Planetary Science, 530 Physics, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Population, black hole physics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radiation, LUMINOSITY FUNCTIONS, LY-ALPHA EMITTERS, 1912 Space and Planetary Science, Ionization, STAR-FORMING GALAXIES, education, Reionization, Astrophysics::Galaxy Astrophysics, media_common, Physics, education.field_of_study, Z-SIMILAR-TO-6 QUASARS, Astrophysics (astro-ph), FORMATION RATE INDICATOR, HYDROGEN REIONIZATION, Universe, diffuse radiation, Black hole, cosmology : theory, 10231 Institute for Computational Science, PROBE WMAP OBSERVATIONS, 3103 Astronomy and Astrophysics, Spectral energy distribution, DIGITAL SKY SURVEY, Halo, intergalactic medium, galaxies : formation, COSMIC REIONIZATION
Abstract

In the pre-reionization Universe, the regions of the inter-galactic medium (IGM) which are far from luminous sources are the last to undergo reionization. Until then, they should be scarcely affected by stellar radiation; instead, the X-ray emission from an early black hole (BH) population can have much larger influence. We investigate the effects of such emission, looking at a number of BH model populations (differing for the cosmological density evolution of BHs, the BH properties, and the spectral energy distribution of the BH emission). We find that BH radiation can easily heat the IGM to 10^3-10^4 K, while achieving partial ionization. The most interesting consequence of this heating is that BHs are expected to induce a 21-cm signal (delta T_b ~ 20-30 mK at z, Comment: 17 pages, 14 figures; accepted for publication on MNRAS

Published
2008

43. Spitzer Imaging of Strongly lensed Herschel-selected Dusty Star-forming Galaxies

Author

Helmut Dannerbauer, Mattia Vaccari, Sébastien Viaene, Joaquin Vieira, Lifan Wang, Duncan Farrah, Dominik A. Riechers, Nicholas Timmons, Hooshang Nayyeri, Asantha Cooray, J. González-Nuevo, Douglas Scott, E. da Cunha, Ivan Oteo, Maarten Baes, Jae Calanog, G. de Zotti, Michał J. Michałowski, Georgios E. Magdis, Hai Fu, Loretta Dunne, Brian Ma, Matthew Smith, Scott Chapman, Julie Wardlow, and Caitlin M. Casey

Subjects
STELLAR MASSES, Stellar mass, PHYSICAL-PROPERTIES, galaxies [submillimeter], FOS: Physical sciences, Flux, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, LUMINOSITY FUNCTIONS, INFRARED GALAXIES, SUBMILLIMETER-SELECTED GALAXIES, EXTRAGALACTIC SURVEY, Astrophysics::Solar and Stellar Astrophysics, Adaptive optics, Astrophysics::Galaxy Astrophysics, QB, Physics, INTERSTELLAR-MEDIUM, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, FORMATION RATES, Galaxy, Redshift, Spire, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), DEEP-FIELD-SOUTH, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, HIGH-REDSHIFT
Abstract

We present the rest-frame optical spectral energy distribution and stellar masses of six Herschel- selected gravitationally lensed dusty, star-forming galaxies (DSFGs) at 1 < z < 3. These galaxies were first identified with Herschel/SPIRE imaging data from the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) and the Herschel Multi-tiered Extragalactic Survey (HerMES). The targets were observed with Spitzer/IRAC at 3.6 and 4.5um. Due to the spatial resolution of the IRAC observations at the level of 2 arcseconds, the lensing features of a background DSFG in the near-infrared are blended with the flux from the foreground lensing galaxy in the IRAC imaging data. We make use of higher resolution Hubble/WFC3 or Keck/NIRC2 Adaptive Optics imaging data to fit light profiles of the foreground lensing galaxy (or galaxies) as a way to model the foreground components, in order to successfully disentangle the foreground lens and background source flux densities in the IRAC images. The flux density measurements at 3.6 and 4.5um, once combined with Hubble/WFC3 and Keck/NIRC2 data, provide important constraints on the rest-frame optical spectral energy distribution of the Herschel-selected lensed DSFGs. We model the combined UV- to millimeter-wavelength SEDs to establish the stellar mass, dust mass, star-formation rate, visual extinction, and other parameters for each of these Herschel-selected DSFGs. These systems have inferred stellar masses in the range 8 x 10^10 to 4 x 10^11 Msun and star-formation rates of around 100 Msun yr-1. This puts these lensed sub-millimeter systems well above the SFR-M* relation observed for normal star-forming galaxies at similar redshifts. The high values of SFR inferred for these systems are consistent with a major merger-driven scenario for star formation., 13 pages, 6 figures, submit to ApJ

Published
2015
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44. H-ATLAS/GAMA:quantifying the morphological evolution of the galaxy population using cosmic calorimetry

Author

Aaron S. G. Robotham, Andrew G. Fullard, Lee S. Kelvin, Christopher J. R. Clark, Douglas Scott, Maarten Baes, Steven Phillipps, Sarah Brough, Claudia Maraston, Stephen Anthony Eales, Edo Ibar, Haley Louise Gomez, Steve Maddox, Andrew M. Hopkins, Asantha Cooray, Steve Serjeant, Elisabetta Valiante, Edward N. Taylor, Jon Loveday, Simon P. Driver, Matthew Allen, Alister W. Graham, Loretta Dunne, Daniel J. Smith, Nathan Bourne, Ivan K. Baldry, Rob Ivison, Matthew Smith, David L. Clements, Paul van der Werf, Simon Dye, Science and Technology Facilities Council (STFC), Science and Technology Facilities Council [2006-2012], and University of St Andrews. School of Physics and Astronomy

Subjects
bulges [galaxies], Astrophysics, 01 natural sciences, Hubble sequence, galaxies: bulges, galaxies: evolution, galaxies: star formation, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QC, media_common, QB, Physics, education.field_of_study, COSMIC cancer database, 3rd-DAS, Physical Sciences, Elliptical galaxy, symbols, astro-ph.CO, Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics, HUBBLE SEQUENCE, Cosmology and Nongalactic Astrophysics (astro-ph.CO), SIMILAR-TO 2, media_common.quotation_subject, astro-ph.GA, Population, MU-M, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, LUMINOSITY FUNCTIONS, galaxies: bulges, symbols.namesake, 0103 physical sciences, STAR-FORMING GALAXIES, education, Astrophysics::Galaxy Astrophysics, evolution [galaxies], STFC, Background radiation, Science & Technology, 010308 nuclear & particles physics, Astronomy, RCUK, Astronomy and Astrophysics, HERSCHEL-ATLAS, DISK GALAXIES, Astrophysics - Astrophysics of Galaxies, Universe, Galaxy, 0201 Astronomical And Space Sciences, Stars, QC Physics, Physics and Astronomy, Space and Planetary Science, galaxies: star formation, Astrophysics of Galaxies (astro-ph.GA), MASS ASSEMBLY GAMA, DIGITAL SKY SURVEY, QUIESCENT GALAXIES, SCIENCE DEMONSTRATION PHASE
Abstract

Using results from the Herschel Astrophysical Terrahertz Large-Area Survey and the Galaxy and Mass Assembly project, we show that, for galaxy masses above approximately 1.0e8 solar masses, 51% of the stellar mass-density in the local Universe is in early-type galaxies (ETGs: Sersic n > 2.5) while 89% of the rate of production of stellar mass-density is occurring in late-type galaxies (LTGs: Sersic n < 2.5). From this zero-redshift benchmark, we have used a calorimetric technique to quantify the importance of the morphological transformation of galaxies over the history of the Universe. The extragalactic background radiation contains all the energy generated by nuclear fusion in stars since the Big Bang. By resolving this background radiation into individual galaxies using the deepest far-infrared survey with the Herschel Space Observatory and a deep near-infrared/optical survey with the Hubble Space Telescope (HST), and using measurements of the Sersic index of these galaxies derived from the HST images, we estimate that approximately 83% of the stellar mass-density formed over the history of the Universe occurred in LTGs. The difference between this and the fraction of the stellar mass-density that is in LTGs today implies there must have been a major transformation of LTGs into ETGs after the formation of most of the stars., Accepted for publication in MNRAS

Published
2015
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45. HERMES: CURRENT COSMIC INFRARED BACKGROUND ESTIMATES CAN BE EXPLAINED BY KNOWN GALAXIES AND THEIR FAINT COMPANIONS AT z \textless 4

Author

Lorenzo Moncelsi, James Dunlop, G. Marsden, Georgios E. Magdis, Ivan Valtchanov, Bernhard Schulz, Matthieu Béthermin, Lucia Marchetti, James J. Bock, Guilaine Lagache, Rob Ivison, L. Conversi, J. Álvarez-Márquez, S. Duivenvoorden, Denis Burgarella, Alberto Franceschini, Michael Zemcov, Mark Halpern, Scott Chapman, Ryan Quadri, Duncan Farrah, Julie Wardlow, David L. Clements, M. J. Page, Ismael Perez-Fournon, S. J. Oliver, A. Conley, Lingyu Wang, Marco P. Viero, Joaquin Vieira, Douglas Scott, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Office National des Forêts (ONF), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre for Fusion Space and Astrophysics [Coventry] (CFSA), University of Warwick [Coventry], AUTRES, University of Colorado [Boulder], Herschel Science Center [Madrid], European Space Astronomy Centre (ESAC), European Space Agency (ESA)-European Space Agency (ESA), Department of Physics [Blacksburg], Virginia Tech [Blacksburg], Dipartimento di Fisica e Astronomia 'Galileo Galilei', Universita degli Studi di Padova, Department of Physics and Astronomy [Vancouver], University of British Columbia (UBC), Royal Observatory Edinburgh (ROE), University of Edinburgh, Service d'Etudes du Comportement des Matériaux de Conditionnement (SECM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), University of Sussex, Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), University of California-University of California, Herschel Science Centre, European Space Agency (ESA), Department of Astronomy, University of California [Irvine] (UCI), California Institute of Technology (CALTECH), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Office national des forêts (ONF), 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), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Università degli Studi di Padova = University of Padua (Unipd), University of California (UC)-University of California (UC), Agence Spatiale Européenne = European Space Agency (ESA), University of California [Irvine] (UC Irvine), Science and Technology Facilities Council (STFC), and Science and Technology Facilities Council [2006-2012]

Subjects
submillimeter: galaxies, Stellar mass, IMAGES, REDSHIFT, Flux, Astrophysics, Astronomy & Astrophysics, LUMINOSITY FUNCTIONS, 01 natural sciences, infrared: galaxies, Cosmic infrared background, 0103 physical sciences, NUMBER COUNTS, 010303 astronomy & astrophysics, large-scale structure of universe, Physics, Science & Technology, SUBMILLIMETER GALAXIES, 010308 nuclear & particles physics, Image (category theory), cosmology: observations, galaxies: evolution, Astronomy and Astrophysics, Space and Planetary Science, STELLAR MASS FUNCTIONS, DUSTY, Astrophysics - Astrophysics of Galaxies, OBSCURED STAR-FORMATION, Galaxy, 0201 Astronomical And Space Sciences, Wavelength, Full width at half maximum, Physical Sciences, DEEP-FIELD-SOUTH, QUIESCENT GALAXIES, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Smoothing
Abstract

We report contributions to cosmic infrared background (CIB) intensities originating from known galaxies and their faint companions at submillimeter wavelengths. Using the publicly-available UltraVISTA catalog, and maps at 250, 350, and 500 {\mu}m from the \emph{Herschel} Multi-tiered Extragalactic Survey (HerMES), we perform a novel measurement that exploits the fact that uncatalogued sources may bias stacked flux densities --- particularly if the resolution of the image is poor --- and intentionally smooth the images before stacking and summing intensities. By smoothing the maps we are capturing the contribution of faint (undetected in K_S ~ 23.4) sources that are physically associated, or correlated, with the detected sources. We find that the cumulative CIB increases with increased smoothing, reaching 9.82 +- 0.78, 5.77 +- 0.43, and 2.32 +- 0.19$\, \rm nW m^{-2} sr^{-1}$ at 250, 350, and 500 {\mu}m at 300 arcsec FWHM. This corresponds to a fraction of the fiducial CIB of 0.94 +- 0.23, 1.07 +- 0.31, and 0.97 +- 0.26 at 250, 350, and 500 {\mu}m, where the uncertainties are dominated by those of the absolute CIB. We then propose, with a simple model combining parametric descriptions for stacked flux densities and stellar mass functions, that emission from galaxies with log(M/Msun) > 8.5 can account for the most of the measured total intensities, and argue against contributions from extended, diffuse emission. Finally, we discuss prospects for future survey instruments to improve the estimates of the absolute CIB levels, and observe any potentially remaining emission at z > 4., Comment: Accepted to ApJL. 6 Pages, 3 figures

Published
2015
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46. New H2O masers in Seyfert and FIR bright galaxies

Subjects
ACTIVE GALACTIC NUCLEI, PARSEC-SCALE JET, ARP 299, MEGAMASER EMISSION, galaxies : active, RADIO STRUCTURES, LUMINOSITY FUNCTIONS, IRAS GALAXIES, galaxies : jets, WATER-VAPOR MASER, NARROW-LINE REGION, galaxies : Seyfert, masers, galaxies : starburst, radio lines : galaxies, VLA OBSERVATIONS
Abstract

Using the Effelsberg 100-m telescope, detections of four extragalactic water vapor masers are reported. Isotropic luminosities are similar to 50, 1000, 1 and 230 L-circle dot for Mrk 1066 ( UGC 2456), Mrk 34, NGC 3556 and Arp 299, respectively. Mrk 34 contains by far the most distant and one of the most luminous water vapor megamasers so far reported in a Seyfert galaxy. The interacting system Arp 299 appears to show two maser hotspots separated by approximately 20''. With these new results and even more recent data from Braatz et al. ( 2004, ApJ, 617, L29), the detection rate in our sample of Seyferts with known jet-Narrow Line Region interactions becomes 50% ( 7/14), while in star forming galaxies with high ( S-100 mu m > 50 Jy) far infrared fluxes the detection rate is 22% (10/45). The jet-NLR interaction sample may not only contain "jet-masers" but also a significant number of accretion "disk-masers" like those seen in NGC4258. A statistical analysis of 53 extragalactic H2O sources ( excluding the Galaxy and the Magellanic Clouds) indicates ( 1) that the correlation between IRAS Point Source and H2O luminosities, established for individual star forming regions in the galactic disk, also holds for AGN-dominated megamaser galaxies; ( 2) that maser luminosities are not correlated with 60 mu m/100 mu m color temperatures; and ( 3) that only a small fraction of the luminous megamasers ( L-H2O > 100 L-circle dot) detectable with 100-m sized telescopes have so far been identified. The H2O luminosity function (LF) suggests that the number of galaxies with 1L(circle dot)

Published
2005
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47. Spitzer Observations of the North Ecliptic Pole

Author

Nayyeri, H., Ghotbi, N., Cooray, A., Bock, J., Clements, D. L., Im, M., Kim, M. G., Korngut, P., Lanz, A., Lee, H. M., Lee, D. H., Malkan, M., Nam, U. W., Pearson, C., Serjeant, S., Smidt, J., Zemcov, M., Matsuhara, Hideo, Matsumoto, Toshio, Matsuura, Shuji, Tsumura, Kohji, and Wada, Takehiko

Subjects
0306 Physical Chemistry (Incl. Structural), Infrared, Young stellar object, Population, FOS: Physical sciences, Ecliptic pole, Astronomy & Astrophysics, LUMINOSITY FUNCTIONS, 0305 Organic Chemistry, 01 natural sciences, infrared: galaxies, Photometry (optics), surveys, GALAXY NUMBER COUNTS, Spitzer Space Telescope, 0103 physical sciences, STAR-FORMING GALAXIES, INFRARED BACKGROUND ANISOTROPIES, SPACE-TELESCOPE, education, infrared: stars, SURVEY STRATEGY, 010303 astronomy & astrophysics, STANDARD STELLAR LIBRARY, Luminous infrared galaxy, Physics, education.field_of_study, Science & Technology, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, DEEP SURVEY, EVOLUTIONARY SYNTHESIS, Astrophysics - Astrophysics of Galaxies, 0201 Astronomical And Space Sciences, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Physical Sciences, Background light, WIDE-FIELD SURVEY
Abstract

著者人数: 22名, Accepted: 2017-11-19, 資料番号: SA1170264000

Published
2018
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48. The zCOSMOS redshift survey : evolution of the light in bulges and discs since z ~ 0.8

Author

Luis C. Ho, O. Le Fevre, H. J. McCracken, P. Franzetti, Anton M. Koekemoer, R. Pello, E. Zucca, A. Cappi, A. Cattaneo, Niraj Welikala, A. Iovino, K. Kovavc, Alvio Renzini, J. F. Le Borgne, R. M. Rich, M. Mignoli, B. Garilli, T. Contini, Yoshiaki Taniguchi, Graziano Coppa, Jean-Paul Kneib, Masaomi Tanaka, C. Lopez-Sanjuan, E. Perez Montero, P. Kampczyk, Vincenzo Mainieri, Andrea Cimatti, F. Lamareille, Richard Massey, Marco Scodeggio, Angela Bongiorno, Rongmon Bordoloi, Y. Peng, L. Tresse, L. A. M. Tasca, C. Knobel, S. Bardelli, Duncan Farrah, Kartik Sheth, Christian Maier, D. Vergani, Michele Moresco, O. Cucciati, S. de la Torre, K. Caputi, C. M. Carollo, M. Bolzonella, Lucia Pozzetti, G. Zamorani, C. T. Liu, D. B. Sanders, Simon J. Lilly, Luigi Guzzo, V. Le Brun, O. Ilbert, Astronomy, Tasca, L.A.M., Tresse, L., Le Fèvre, O., Ilbert, O., Lilly, S.J., Zamorani, G., López-Sanjuan, C., Ho, L.C., Bardelli, S., Cattaneo, A., Cucciati, O., Farrah, D., Iovino, A., Koekemoer, A.M., Liu, C.T., Massey, R., Renzini, A., Taniguchi, Y., Welikala, N., Zucca, E., Carollo, C.M., Contini, T., Kneib, J.-P., Mainieri, V., Scodeggio, M., Bolzonella, M., Bongiorno, A., Caputi, K., De La Torre, S., Franzetti, P., Garilli, B., Guzzo, L., Kampczyk, P., Knobel, C., Kovač, K., Lamareille, F., Le Borgne, J.-F., Le Brun, V., Maier, C., Mignoli, M., Pello, R., Peng, Y., Perez Montero, E., Rich, R.M., Tanaka, M., Vergani, D., Bordoloi, R., Cappi, A., Cimatti, A., Coppa, G., Mccracken, H.J., Moresco, M., Pozzetti, L., Sanders, D., and Sheth, K.

Subjects
Galaxies: fundamental parameter, FORMING GALAXY, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, fundamental parameters. [Galaxies], LUMINOSITY FUNCTIONS, galaxies: bulges, STAR-FORMATION RATE, Luminosity, ADVANCED CAMERA, bulges [Galaxies], Bulge, distances and redshifts [Galaxies], Galaxies: distances and redshift, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Physics, FORMATION HISTORY, Star formation, Astronomy and Astrophysics, galaxies: fundamental parameters, HUBBLE-SPACE-TELESCOPE, VLT DEEP SURVEY, Astronomy and Astrophysic, Redshift survey, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, luminosity function [Galaxies], Redshift, Galaxy, Stars, galaxies: luminosity function, Space and Planetary Science, mass function, Astrophysics of Galaxies (astro-ph.GA), galaxies: luminosity function, mass function, Astrophysics::Earth and Planetary Astrophysics, GALAXY FORMATION, galaxies: distances and redshifts, Irregular galaxy, galaxies: evolution, Galaxies: bulge, SURVEY COSMOS
Abstract

We studied the chronology of galactic bulge and disc formation by analysing the relative contributions of these components to the B-band rest-frame luminosity density at different epochs. We present the first estimate of the evolution of the fraction of rest-frame B-band light in galactic bulges and discs since redshift z~0.8. We performed a bulge-to-disc decomposition of HST/ACS images of 3266 galaxies in the zCOSMOS-bright survey with spectroscopic redshifts in the range 0.7 < z < 0.9. We find that the fraction of B-band light in bulges and discs is $(26 \pm 4)%$ and $(74 \pm 4)%$, respectively. When compared with rest-frame B-band measurements of galaxies in the local Universe in the same mass range ($10^{9} M_{\odot}\lessapprox M \lessapprox 10^{11.5} M_{\odot}$), we find that the B-band light in discs decreases by ~30% from z~0.7-0.9 to z~0, while the light from the bulge increases by ~30% over the same period of time. We interpret this evolution as the consequence of star formation and mass assembly processes, as well as morphological transformation, which gradually shift stars formed at half the age of the Universe from star-forming late-type/irregular galaxies toearlier types and ultimately into spheroids., Letter to the Editor, 4 pages, 2 figures, accepted for publication in Astronomy and Astrophysics

Published
2014

49. On the evolutionary behaviour of BL Lac objects

Subjects
ACTIVE GALACTIC NUCLEI, GALAXIES, POLARIZATION, SAMPLE, X-rays : galaxies, Astrophysics::High Energy Astrophysical Phenomena, galaxies : active, CONSTRAINTS, Astrophysics::Cosmology and Extragalactic Astrophysics, BL Lacertae objects : general, LUMINOSITY FUNCTIONS, LACERTAE OBJECTS
Abstract

We present a new well defined sample of BL Lac objects selected from the ROSAT All-Sky Survey (RASS). The sample consists of 39 objects with 35 forming a flux limited sample down to f(X) (0.5 - 2.0 keV) = 8 . 10(-13) ergs cm(-2) s(-1); redshifts are known for 33 objects (and 31 of the complete sample). X-ray spectral properties were determined for each object individually with the RASS data. The luminosity function of RASS selected BL Lac objects is compatible with results provided by objects selected with the Einstein observatory, but the RASS selected sample contains objects with luminosities at least tenfold higher. Our analysis confirms the negative evolution for X-ray selected BL Lac objects found in a sample by the Einstein observatory, the parameterization provides similar results. A subdivision of the sample into halves according to the X-ray to optical flux ratio yielded unexpected results. The extremely X-ray dominated objects have higher redshifts and X-ray luminosities and only this subgroup shows clear signs of strong negative evolution. The evolutionary behaviour of objects with an intermediate spectral energy distribution between X-ray and radio dominated is compatible with no evolution at all. Consequences for unified schemes of X-ray and radio selected BL Lac objects are discussed. We suggest that the intermediate BL Lac objects are the basic BL Lac population. The distinction between the two subgroups can be explained if extremely X-ray dominated BL Lac objects are observed in a state of enhanced X-ray activity.

Published
1998

50. Galaxy And Mass Assembly (GAMA) : the large-scale structure of galaxies and comparison to mock universes

Author

T. Mcnaught-Roberts, Jochen Liske, Simon P. Driver, Jon Loveday, Matthew Colless, Maritza A. Lara-López, Kevin A. Pimbblet, Alex Merson, Mehmet Alpaslan, Peder Norberg, Andrew M. Hopkins, Aaron S. G. Robotham, Angel R. Lopez-Sanchez, Michelle E. Cluver, Eelco van Kampen, Ivan K. Baldry, Caroline Foster, Amanda E. Bauer, Joss Bland-Hawthorn, Michael J. I. Brown, Lee S. Kelvin, and University of St Andrews. School of Physics and Astronomy

Subjects
Morphology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Cosmic web, Luminosity functions, FOS: Physical sciences, Library science, Voids, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Filaments, Clusters, Scale structure, QB Astronomy, observational [Methods], Astrophysics::Galaxy Astrophysics, QB, Physics, Receipt, European research, Astronomy, Astronomy and Astrophysics, Superstructures, Classification, Methods observational, Space and Planetary Science, Research council, Redshift survey, Catalog, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

From a volume limited sample of 45,542 galaxies and 6,000 groups with $z \leq 0.213$ we use an adapted minimal spanning tree algorithm to identify and classify large scale structures within the Galaxy and Mass Assembly (GAMA) survey. Using galaxy groups, we identify 643 filaments across the three equatorial GAMA fields that span up to 200 $h^{-1}$ Mpc in length, each with an average of 8 groups within them. By analysing galaxies not belonging to groups we identify a secondary population of smaller coherent structures composed entirely of galaxies, dubbed `tendrils' that appear to link filaments together, or penetrate into voids, generally measuring around 10 $h^{-1}$ Mpc in length and containing on average 6 galaxies. Finally we are also able to identify a population of isolated void galaxies. By running this algorithm on GAMA mock galaxy catalogues we compare the characteristics of large scale structure between observed and mock data; finding that mock filaments reproduce observed ones extremely well. This provides a probe of higher order distribution statistics not captured by the popularly used two-point correlation function., Comment: 20 pages, 16 figures, accepted for publication in the Monthly Notices of the Royal Astronomical Society

Published
2014

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