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209 results on '"Almaini, Omar"'

201. Minor versus major mergers: the stellar mass growth of massive galaxies from z=3 using number density selection techniques

Author

Ownsworth, Jamie R., Conselice, Christopher J., Mortlock, Alice, Hartley, William G., Almaini, Omar, Duncan, Ken, Mundy, Carl J., Ownsworth, Jamie R., Conselice, Christopher J., Mortlock, Alice, Hartley, William G., Almaini, Omar, Duncan, Ken, and Mundy, Carl J.

Abstract

We present a study on the stellar mass growth of the progenitors of local massive galaxies with a variety of number density selections with n≤1×10−4 Mpc−3 (corresponding to M*=1011.24 M⊙ at z=0.3) in the redshift range 0.3

202. Galaxy Zoo: CANDELS barred discs and bar fractions

Author

Simmons, B. D., Melvin, Thomas, Lintott, Chris, Masters, Karen L., Willett, Kyle W., Keel, William C., Smethurst, R. J., Cheung, Edmond, Nichol, Robert C., Schawinski, Kevin, Rutkowski, Michael, Kartaltepe, Jeyhan S., Bell, Eric F., Casteels, Kevin R. V., Conselice, Christopher J., Almaini, Omar, Ferguson, Henry C., Fortson, Lucy, Hartley, William, Kocevski, Dale, Koekemoer, Anton M., McIntosh, Daniel H., Mortlock, Alice, Newman, Jeffrey A., Ownsworth, Jamie, Bamford, Steven, Dahlen, Tomas, Faber, Sandra M., Finkelstein, Steven L., Fontana, Adriano, Galametz, Audrey, Grogin, N. A., Grützbauch, Ruth, Guo, Yicheng, Häußler, Boris, Jek, Kian J., Kaviraj, Sugata, Lucas, Ray A., Peth, Michael, Salvato, Mara, Wiklind, Tommy, Wuyts, Stijn, Simmons, B. D., Melvin, Thomas, Lintott, Chris, Masters, Karen L., Willett, Kyle W., Keel, William C., Smethurst, R. J., Cheung, Edmond, Nichol, Robert C., Schawinski, Kevin, Rutkowski, Michael, Kartaltepe, Jeyhan S., Bell, Eric F., Casteels, Kevin R. V., Conselice, Christopher J., Almaini, Omar, Ferguson, Henry C., Fortson, Lucy, Hartley, William, Kocevski, Dale, Koekemoer, Anton M., McIntosh, Daniel H., Mortlock, Alice, Newman, Jeffrey A., Ownsworth, Jamie, Bamford, Steven, Dahlen, Tomas, Faber, Sandra M., Finkelstein, Steven L., Fontana, Adriano, Galametz, Audrey, Grogin, N. A., Grützbauch, Ruth, Guo, Yicheng, Häußler, Boris, Jek, Kian J., Kaviraj, Sugata, Lucas, Ray A., Peth, Michael, Salvato, Mara, Wiklind, Tommy, and Wuyts, Stijn

Abstract

The formation of bars in disc galaxies is a tracer of the dynamical maturity of the population. Previous studies have found that the incidence of bars in discs decreases from the local Universe to z ∼ 1, and by z>1 simulations predict that bar features in dynamically mature discs should be extremely rare. Here, we report the discovery of strong barred structures in massive disc galaxies at z ∼ 1.5 in deep rest-frame optical images from the Cosmic Assembly Near-Infrared Deep Extragalactic Legacy Survey. From within a sample of 876 disc galaxies identified by visual classification in Galaxy Zoo, we identify 123 barred galaxies. Selecting a subsample within the same region of the evolving galaxy luminosity function (brighter than L*), we find that the bar fraction across the redshift range 0.5 ≤ z ≤ 2 ( $f_{{\rm bar}} = 10.7^{+6.3}_{-3.5}$ per cent after correcting for incompleteness) does not significantly evolve. We discuss the implications of this discovery in the context of existing simulations and our current understanding of the way disc galaxies have evolved over the last 11 billion years

203. Evidence for a large fraction of Compton-thick quasars at high redshift.

Author

Martínez-Sansigre, Alejo, Rawlings, Steve, Bonfield, David G., Mateos, Silvia, Simpson, Chris, Watson, Mike, Almaini, Omar, Foucaud, Sébastien, Sekiguchi, Kazuhiro, and Ueda, Yoshihiro

Subjects
QUASARS, REDSHIFT, STARBURSTS, SPECTRAL energy distribution, GALACTIC nuclei, X-ray astronomy
Abstract

Using mid-infrared and radio selection criteria, we pre-select a sample of candidate high-redshift type 2 quasars in the Subaru XMM–Newton Deep Field (SXDF). To filter out starburst contaminants, we use a Bayesian method to fit the spectral energy distributions (SEDs) between 24-μm and the B-band, obtain photometric redshifts, and identify the best candidates for high- z type 2 quasars. This leaves us with type 2 quasar candidates in an area ∼0.8 deg2, of which only two have secure X-ray detections. The two detected sources have estimated column densities & , i.e. heavily obscured but Compton-thin quasars. Given the large bolometric luminosities and redshifts of the undetected objects, the lack of X-ray detections suggests extreme absorbing columns are typical. We have found evidence for a population of ‘Compton-thick’ high-redshift type 2 quasars, at least comparable to, and probably larger than, the type 1 quasar population, although spectroscopic confirmation of their active galactic nuclei nature is important. [ABSTRACT FROM AUTHOR]

Published
2007
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204. The Physical Conditions of Emission-line Galaxies at Cosmic Dawn from JWST/NIRSpec Spectroscopy in the SMACS 0723 Early Release Observations

Author

Jonathan R. Trump, Pablo Arrabal Haro, Raymond C. Simons, Bren E. Backhaus, Ricardo O. Amorín, Mark Dickinson, Vital Fernández, Casey Papovich, David C. Nicholls, Lisa J. Kewley, Samantha W. Brunker, John J. Salzer, Stephen M. Wilkins, Omar Almaini, Micaela B. Bagley, Danielle A. Berg, Rachana Bhatawdekar, Laura Bisigello, Véronique Buat, Denis Burgarella, Antonello Calabrò, Caitlin M. Casey, Laure Ciesla, Nikko J. Cleri, Justin W. Cole, M. C. Cooper, Asantha R. Cooray, Luca Costantin, Darren Croton, Henry C. Ferguson, Steven L. Finkelstein, Seiji Fujimoto, Jonathan P. Gardner, Eric Gawiser, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Marc Huertas-Company, Taylor A. Hutchison, Shardha Jogee, Stéphanie Juneau, Intae Jung, Jeyhan S. Kartaltepe, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Jennifer M. Lotz, Ray A. Lucas, Benjamin Magnelli, Jasleen Matharu, Pablo G. Pérez-González, Nor Pirzkal, Marc Rafelski, Caitlin Rose, Lise-Marie Seillé, Rachel S. Somerville, Amber N. Straughn, Sandro Tacchella, Brittany N. Vanderhoof, Benjamin J. Weiner, Stijn Wuyts, L. Y. Aaron Yung, Jorge A. Zavala, Trump, Jonathan R [0000-0002-1410-0470], Haro, Pablo Arrabal [0000-0002-7959-8783], Simons, Raymond C [0000-0002-6386-7299], Backhaus, Bren E [0000-0001-8534-7502], Amorín, Ricardo O [0000-0001-5758-1000], Dickinson, Mark [0000-0001-5414-5131], Fernández, Vital [0000-0003-0531-5450], Papovich, Casey [0000-0001-7503-8482], Nicholls, David C [0000-0003-0892-5203], Kewley, Lisa J [0000-0001-8152-3943], Brunker, Samantha W [0000-0001-6776-2550], Salzer, John J [0000-0001-8483-603X], Wilkins, Stephen M [0000-0003-3903-6935], Almaini, Omar [0000-0001-9328-3991], Bagley, Micaela B [0000-0002-9921-9218], Berg, Danielle A [0000-0002-4153-053X], Bhatawdekar, Rachana [0000-0003-0883-2226], Bisigello, Laura [0000-0003-0492-4924], Buat, Véronique [0000-0003-3441-903X], Burgarella, Denis [0000-0002-4193-2539], Calabrò, Antonello [0000-0003-2536-1614], Casey, Caitlin M [0000-0002-0930-6466], Ciesla, Laure [0000-0003-0541-2891], Cleri, Nikko J [0000-0001-7151-009X], Cole, Justin W [0000-0002-6348-1900], Cooper, MC [0000-0003-1371-6019], Cooray, Asantha R [0000-0002-3892-0190], Costantin, Luca [0000-0001-6820-0015], Croton, Darren [0000-0002-5009-512X], Ferguson, Henry C [0000-0001-7113-2738], Finkelstein, Steven L [0000-0001-8519-1130], Fujimoto, Seiji [0000-0001-7201-5066], Gardner, Jonathan P [0000-0003-2098-9568], Gawiser, Eric [0000-0003-1530-8713], Giavalisco, Mauro [0000-0002-7831-8751], Grazian, Andrea [0000-0002-5688-0663], Grogin, Norman A [0000-0001-9440-8872], Hathi, Nimish P [0000-0001-6145-5090], Hirschmann, Michaela [0000-0002-3301-3321], Holwerda, Benne W [0000-0002-4884-6756], Huertas-Company, Marc [0000-0002-1416-8483], Hutchison, Taylor A [0000-0001-6251-4988], Jogee, Shardha [0000-0002-1590-0568], Juneau, Stéphanie [0000-0002-0000-2394], Jung, Intae [0000-0003-1187-4240], Kartaltepe, Jeyhan S [0000-0001-9187-3605], Kirkpatrick, Allison [0000-0002-1306-1545], Kocevski, Dale D [0000-0002-8360-3880], Koekemoer, Anton M [0000-0002-6610-2048], Lotz, Jennifer M [0000-0003-3130-5643], Lucas, Ray A [0000-0003-1581-7825], Magnelli, Benjamin [0000-0002-6777-6490], Matharu, Jasleen [0000-0002-7547-3385], Pérez-González, Pablo G [0000-0003-4528-5639], Pirzkal, Nor [0000-0003-3382-5941], Rafelski, Marc [0000-0002-9946-4731], Rose, Caitlin [0000-0002-8018-3219], Seillé, Lise-Marie [0000-0001-7755-4755], Somerville, Rachel S [0000-0002-6748-6821], Straughn, Amber N [0000-0002-4772-7878], Tacchella, Sandro [0000-0002-8224-4505], Vanderhoof, Brittany N [0000-0002-8163-0172], Weiner, Benjamin J [0000-0001-6065-7483], Wuyts, Stijn [0000-0003-3735-1931], Aaron Yung, LY [0000-0003-3466-035X], Zavala, Jorge A [0000-0002-7051-1100], Apollo - University of Cambridge Repository, Trump, JR [0000-0002-1410-0470], Haro, PA [0000-0002-7959-8783], Simons, RC [0000-0002-6386-7299], Backhaus, BE [0000-0001-8534-7502], Amorín, RO [0000-0001-5758-1000], Dickinson, M [0000-0001-5414-5131], Fernández, V [0000-0003-0531-5450], Papovich, C [0000-0001-7503-8482], Nicholls, DC [0000-0003-0892-5203], Kewley, LJ [0000-0001-8152-3943], Brunker, SW [0000-0001-6776-2550], Salzer, JJ [0000-0001-8483-603X], Wilkins, SM [0000-0003-3903-6935], Almaini, O [0000-0001-9328-3991], Bagley, MB [0000-0002-9921-9218], Berg, DA [0000-0002-4153-053X], Bhatawdekar, R [0000-0003-0883-2226], Bisigello, L [0000-0003-0492-4924], Buat, V [0000-0003-3441-903X], Burgarella, D [0000-0002-4193-2539], Calabrò, A [0000-0003-2536-1614], Casey, CM [0000-0002-0930-6466], Ciesla, L [0000-0003-0541-2891], Cleri, NJ [0000-0001-7151-009X], Cole, JW [0000-0002-6348-1900], Cooray, AR [0000-0002-3892-0190], Costantin, L [0000-0001-6820-0015], Croton, D [0000-0002-5009-512X], Ferguson, HC [0000-0001-7113-2738], Finkelstein, SL [0000-0001-8519-1130], Fujimoto, S [0000-0001-7201-5066], Gardner, JP [0000-0003-2098-9568], Gawiser, E [0000-0003-1530-8713], Giavalisco, M [0000-0002-7831-8751], Grazian, A [0000-0002-5688-0663], Grogin, NA [0000-0001-9440-8872], Hathi, NP [0000-0001-6145-5090], Hirschmann, M [0000-0002-3301-3321], Holwerda, BW [0000-0002-4884-6756], Huertas-Company, M [0000-0002-1416-8483], Hutchison, TA [0000-0001-6251-4988], Jogee, S [0000-0002-1590-0568], Juneau, S [0000-0002-0000-2394], Jung, I [0000-0003-1187-4240], Kartaltepe, JS [0000-0001-9187-3605], Kirkpatrick, A [0000-0002-1306-1545], Kocevski, DD [0000-0002-8360-3880], Koekemoer, AM [0000-0002-6610-2048], Lotz, JM [0000-0003-3130-5643], Lucas, RA [0000-0003-1581-7825], Magnelli, B [0000-0002-6777-6490], Matharu, J [0000-0002-7547-3385], Pérez-González, PG [0000-0003-4528-5639], Pirzkal, N [0000-0003-3382-5941], Rafelski, M [0000-0002-9946-4731], Rose, C [0000-0002-8018-3219], Seillé, LM [0000-0001-7755-4755], Somerville, RS [0000-0002-6748-6821], Straughn, AN [0000-0002-4772-7878], Tacchella, S [0000-0002-8224-4505], Vanderhoof, BN [0000-0002-8163-0172], Weiner, BJ [0000-0001-6065-7483], Wuyts, S [0000-0003-3735-1931], and Zavala, JA [0000-0002-7051-1100]

Subjects
similar-to 2, SIMILAR-TO 2, NEAR-INFRARED SPECTROSCOPY, COLLISION STRENGTHS, near-infrared spectroscopy, MASS-METALLICITY RELATION, FOS: Physical sciences, CHEMICAL-COMPOSITION, Galaxies and Cosmology, collision strengths, LY-ALPHA, atomic database, STAR-FORMING GALAXIES, MOSDEF SURVEY, mosdef survey, NEBULAR EMISSION, Astronomy and Astrophysics, mass-metallicity relation, star-forming galaxies, Astrophysics - Astrophysics of Galaxies, ATOMIC DATABASE, ly-alpha, nebular emission, Space and Planetary Science, 5101 Astronomical Sciences, Astrophysics of Galaxies (astro-ph.GA), chemical-composition, 51 Physical Sciences
Abstract

We present rest-frame optical emission-line flux ratio measurements for five $z>5$ galaxies observed by the JWST Near-Infared Spectrograph (NIRSpec) in the SMACS 0723 Early Release Observations. We add several quality-control and post-processing steps to the NIRSpec pipeline reduction products in order to ensure reliable relative flux calibration of emission lines that are closely separated in wavelength, despite the uncertain \textit{absolute} spectrophotometry of the current version of the reductions. Compared to $z\sim3$ galaxies in the literature, the $z>5$ galaxies have similar [OIII]$\lambda$5008/H$\beta$ ratios, similar [OIII]$\lambda$4364/H$\gamma$ ratios, and higher ($\sim$0.5 dex) [NeIII]$\lambda$3870/[OII]$\lambda$3728 ratios. We compare the observations to MAPPINGS V photoionization models and find that the measured [NeIII]$\lambda$3870/[OII]$\lambda$3728, [OIII]$\lambda$4364/H$\gamma$, and [OIII]$\lambda$5008/H$\beta$ emission-line ratios are consistent with an interstellar medium that has very high ionization ($\log(Q) \simeq 8-9$, units of cm~s$^{-1}$), low metallicity ($Z/Z_\odot \lesssim 0.2$), and very high pressure ($\log(P/k) \simeq 8-9$, units of cm$^{-3}$). The combination of [OIII]$\lambda$4364/H$\gamma$ and [OIII]$\lambda$(4960+5008)/H$\beta$ line ratios indicate very high electron temperatures of $4.1, Comment: Accepted for publication in AAS Journals. 14 pages, 6 figures, 3 tables

Published
2023
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205. Growing up in a megalopolis: environmental effects on galaxy evolution in a supercluster at z~0.65 in UKIDSS UDS.

Author

Galametz, Audrey, Pentericci, Laura, Castellano, Marco, Mendel, Trevor, Hartley, Will G., Fossati, Matteo, Finoguenov, Alexis, Almaini, Omar, Beifiori, Alessandra, Fontana, Adriano, Grazian, Andrea, Scodeggio, Marco, and Kocevski, Dale D.

Subjects
*GALACTIC evolution, *SUPERGIANT stars, *STAR formation, *GALAXY clusters, *SUPERCLUSTERS, *SPECTRUM analysis
Abstract

We present a large-scale galaxy structure Cl J021734-0513 at z~ 0.65 discovered in the UKIDSS UDS field, made of~20 galaxy groups and clusters, spreading over 10Mpc. We report on a VLT/VIMOS spectroscopic follow-up program that, combined with past spectroscopy, allowed us to confirm four galaxy clusters (M200~ 1014 M~) and a dozen associated groups and star-forming galaxy overdensities. Two additional filamentary structures at z~0.62 and 0.69 and foreground and background clusters at 0.6 < z < 0.7 were also confirmed along the line of sight. The structure subcomponents are at different formation stages. The clusters have a core dominated by passive galaxies and an established red sequence. The remaining structures are a mix of star-forming galaxy overdensities and forming groups. The presence of quiescent galaxies in the core of the latter shows that 'pre-processing' has already happened before the groups fall into theirmoremassive neighbours. Our spectroscopy allows us to derive spectral index measurements e.g. emission/absorption line equivalent widths, strength of the 4000Å break, valuable to investigate the star formation history of structure members. Based on these line measurements, we select a population of 'post-starburst' galaxies. These galaxies are preferentially found within the virial radius of clusters, supporting a scenario in which their recent quenching could be prompted by gas stripping by the dense intracluster medium. We derive stellar age estimates using Markov Chain Monte Carlo-based spectral fitting for quiescent galaxies and find a correlation between ages and colours/stellar masses which favours a top-down formation scenario of the red sequence. A catalogue of~650 redshifts in UDS is released alongside the paper (via MNRAS online data). [ABSTRACT FROM AUTHOR]

Published
2018
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207. CANDELS OBSERVATIONS OF THE ENVIRONMENTAL DEPENDENCE OF THE COLOR–MASS–MORPHOLOGY RELATION AT z = 1.6.

Author

BASSETT, ROBERT, PAPOVICH, CASEY, LOTZ, JENNIFER M., BELL, ERIC F., FINKELSTEIN, STEVEN L., NEWMAN, JEFFREY A., TRAN, KIM-VY, ALMAINI, OMAR, LANI, CATERINA, COOPER, MICHAEL, CROTON, DARREN, DEKEL, AVISHAI, FERGUSON, HENRY C., KOCEVSKI, DALE D., KOEKEMOER, ANTON M., KOO, DAVID C., MCGRATH, ELIZABETH J., MCINTOSH, DANIEL H., and WECHSLER, RISA

Subjects
*STELLAR mass, *NEAR infrared radiation, *QUIESCENT plasmas, *GALAXY clusters, *REDSHIFT
Abstract

We study the environmental dependence of color, stellar mass, and morphology by comparing galaxies in a forming cluster to those in the field at z = 1.6 with Hubble Space Telescope near-infrared imaging in the CANDELS/UDS field. We quantify the morphology of the galaxies using the effective radius, reff , and Sérsic index, n. In both the cluster and field, approximately half of the bulge-dominated galaxies (n > 2) reside on the red sequence of the color-magnitude diagram, and most disk-dominated galaxies (n < 2) have colors expected for star-forming galaxies. There is weak evidence that cluster galaxies have redder rest-frame U-B colors and higher stellar masses compared to the field. Star-forming galaxies in both the cluster and field show no significant differences in their morphologies. In contrast, there is evidence that quiescent galaxies in the cluster have larger median effective radii and smaller Sérsic indices compared to the field with a significance of 2σ. These differences are most pronounced for galaxies at clustercentric distances 1Mpc< Rproj < 1.5Mpc, which have low Sérsic indices and possibly larger effective radii, more consistent with star-forming galaxies at this epoch and in contrast to other quiescent galaxies. We argue that star-forming galaxies are processed under the influence of the cluster environment at distances greater than the cluster-halo virial radius. Our results are consistent with models where gas accretion onto these galaxies is suppressed from processes associated with the cluster environment. [ABSTRACT FROM AUTHOR]

Published
2013
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208. High-velocity outflows in massive post-starburst galaxies at z > 1

Author

Ricardo Amorín, Nina A. Hatch, Anton M. Koekemoer, Kate Rowlands, Fabio Fontanot, Andrea Cimatti, Bianca Garilli, Fergus Cullen, James Dunlop, Vivienne Wild, Ross J. McLure, William G. Hartley, Margherita Talia, David T. Maltby, Miguel Socolovsky, D. J. McLeod, Giovanni Cresci, A. C. Carnall, Omar Almaini, Marco Castellano, Aaron Wilkinson, Laura Pentericci, E. J. Bradshaw, Stephane de Barros, Maltby, David T, Almaini, Omar, McLure, Ross J, Wild, Vivienne, Dunlop, Jame, Rowlands, Kate, Hartley, William G, Hatch, Nina A, Socolovsky, Miguel, Wilkinson, Aaron, Amorin, Ricardo, Bradshaw, Emma J, Carnall, Adam C, Castellano, Marco, Cimatti, Andrea, Cresci, Giovanni, Cullen, Fergu, De Barros, Stephane, Fontanot, Fabio, Garilli, Bianca, Koekemoer, Anton M, McLeod, Derek J, Pentericci, Laura, Talia, Margherita, and University of St Andrews. School of Physics and Astronomy

Subjects
Active galactic nucleus, astro-ph.GA, High velocity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, high-redshift [Galaxies], galaxies: high-redshift, 0103 physical sciences, ISM [Galaxies], QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, Absorption (logic), 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, QB, Physics, 010308 nuclear & particles physics, kinematics and dynamics [Galaxies], Sigma, Velocity dispersion, Astronomy and Astrophysics, 3rd-DAS, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Interstellar medium, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: ISM
Abstract

We investigate the prevalence of galactic-scale outflows in post-starburst (PSB) galaxies at high redshift ($1 < z < 1.4$), using the deep optical spectra available in the UKIDSS Ultra Deep Survey (UDS). We use a sample of $\sim40$ spectroscopically confirmed PSBs, recently identified in the UDS field, and perform a stacking analysis in order to analyse the structure of strong interstellar absorption features such as Mg ii ($\lambda2800$ Ang.). We find that for massive ($M_* > 10^{10}\rm\,M_{\odot}$) PSBs at $z > 1$, there is clear evidence for a strong blue-shifted component to the Mg ii absorption feature, indicative of high-velocity outflows ($v_{\rm out}\sim1150\pm160\rm\,km\,s^{-1}$) in the interstellar medium. We conclude that such outflows are typical in massive PSBs at this epoch, and potentially represent the residual signature of a feedback process that quenched these galaxies. Using full spectral fitting, we also obtain a typical stellar velocity dispersion $��_*$ for these PSBs of $\sim200\rm\,km\,s^{-1}$, which confirms they are intrinsically massive in nature (dynamical mass $M_{\rm d}\sim10^{11}\rm\,M_{\odot}$). Given that these high-$z$ PSBs are also exceptionally compact ($r_{\rm e}\sim1$--$2\rm\,kpc$) and spheroidal (Sersic index $n\sim3$), we propose that the outflowing winds may have been launched during a recent compaction event (e.g. major merger or disc collapse) that triggered either a centralised starburst or active galactic nuclei (AGN) activity. Finally, we find no evidence for AGN signatures in the optical spectra of these PSBs, suggesting they were either quenched by stellar feedback from the starburst itself, or that if AGN feedback is responsible, the AGN episode that triggered quenching does not linger into the post-starburst phase., 13 pages, 6 figures, accepted for publication in MNRAS

Published
2019
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209. X-UDS: The Chandra Legacy Survey of the UKIDSS Ultra Deep Survey Field

Author

Anton M. Koekemoer, Rachel S. Somerville, Roberto Gilli, Yoshihiro Ueda, Nico Cappelluti, Dale D. Kocevski, Yuxuan Li, John D. Silverman, Antonis Georgakakis, Takamitsu Miyaji, James Aird, Alexis Finoguenov, Mara Salvato, Andrea Comastri, David M. Alexander, Yanxia Li, Murray Brightman, James Mullaney, Christopher J. Conselice, Francesca Civano, M. Dickinson, Omar Almaini, Johannes Buchner, Casey Papovich, Guenther Hasinger, David J. Rosario, Marcella Brusa, Kirpal Nandra, Kocevski Dale D., Hasinger Guenther , Brightman Murray , Nandra Kirpal , Georgakakis Antonis , Cappelluti Nico , Civano Francesca , Li Yuxuan , Li Yanxia , Aird James , Alexander David M. , Almaini Omar , Brusa Marcella , Buchner Johannes , Comastri ,rea , Conselice Christopher J. , Dickinson Mark A. , Finoguenov Alexis , Gilli Roberto , Koekemoer Anton M. , Miyaji Takamitsu , Mullaney James R. , Papovich Casey , Rosario David , Salvato Mara , Silverman John D. , Somerville Rachel S. , Ueda Yoshihiro, Doctoral Programme in Particle Physics and Universe Sciences, and Department of Physics

Subjects
ACTIVE GALACTIC NUCLEI, SELECTION, RAY DATA, Active galactic nucleus, Field (physics), Point source, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Poisson distribution, 01 natural sciences, Luminosity, symbols.namesake, surveys, SUPERMASSIVE BLACK-HOLES, 0103 physical sciences, LIKELIHOOD RATIO, GROTH STRIP, survey, Fraction (mathematics), NUMBER COUNTS, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, GALAXY MERGERS, Astronomy and Astrophysics, FLUCTUATIONS, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, EVOLUTION, Redshift, X-rays: galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, galaxies: nuclei, Data reduction
Abstract

We present the X-UDS survey, a set of wide and deep Chandra observations of the Subaru-XMM Deep/UKIDSS Ultra Deep Survey (SXDS/UDS) field. The survey consists of 25 observations that cover a total area of 0.33 deg$^{2}$. The observations are combined to provide a nominal depth of ~600 ksec in the central 100 arcmin$^{2}$ region of the field that has been imaged with Hubble/WFC3 by the CANDELS survey and $\sim$200 ksec in the remainder of the field. In this paper, we outline the survey's scientific goals, describe our observing strategy, and detail our data reduction and point source detection algorithms. Our analysis has resulted in a total of 868 band-merged point sources detected with a false-positive Poisson probability of $, 15 pages, 11 figures, published in the Astrophysics Journal Supplement Series

Published
2018

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