Search

Your search keyword '"Driver, Simon"' showing total 307 results
Start Over Author "Driver, Simon" Journal monthly notices of the royal astronomical society
307 results on '"Driver, Simon"'

1. DEVILS/MIGHTEE/GAMA/DINGO: The impact of SFR timescales on the SFR-radio luminosity correlation

Author

Cook, Robin H W, primary, Davies, Luke J M, additional, Rhee, Jonghwan, additional, Hale, Catherine L, additional, Bellstedt, Sabine, additional, Thorne, Jessica E, additional, Delvecchio, Ivan, additional, Collier, Jordan D, additional, Dodson, Richard, additional, Driver, Simon P, additional, Holwerda, Benne W, additional, Jarvis, Matt J, additional, Knowles, Kenda, additional, Lagos, Claudia, additional, Maddox, Natasha, additional, Meyer, Martin, additional, Robotham, Aaron S G, additional, Roychowdhury, Sambit, additional, Rozgonyi, Kristof, additional, Seymour, Nicholas, additional, Siudek, Malgorzata, additional, Whiting, Matthew, additional, and Whittam, Imogen, additional

Published
2024
Full Text
View/download PDF

3. DEVILS/MIGHTEE/GAMA/DINGO: the impact of SFR time-scales on the SFR-radio luminosity correlation.

Author

Cook, Robin H W, Davies, Luke J M, Rhee, Jonghwan, Hale, Catherine L, Bellstedt, Sabine, Thorne, Jessica E, Delvecchio, Ivan, Collier, Jordan D, Dodson, Richard, Driver, Simon P, Holwerda, Benne W, Jarvis, Matt J, Knowles, Kenda, Lagos, Claudia, Maddox, Natasha, Meyer, Martin, Robotham, Aaron S G, Roychowdhury, Sambit, Rozgonyi, Kristof, and Seymour, Nicholas

Subjects
DINGO, SYNCHROTRON radiation, SPECTRAL energy distribution, LUMINOSITY, STARS, COSMIC rays, STAR formation
Abstract

The tight relationship between infrared luminosity (L TIR) and 1.4 GHz radio continuum luminosity (⁠|$L_\mathrm{1.4\, GHz}$|⁠) has proven useful for understanding star formation free from dust obscuration. Infrared emission in star-forming galaxies typically arises from recently formed, dust-enshrouded stars, whereas radio synchrotron emission is expected from subsequent supernovae. By leveraging the wealth of ancillary far-ultraviolet – far-infrared photometry from the Deep Extragalactic VIsible Legacy Survey and Galaxy and Mass Assembly surveys, combined with 1.4 GHz observations from the Meer Karoo Array Telescope International GHz Tiered Extragalactic Exploration survey and Deep Investigation of Neutral Gas Origin projects, we investigate the impact of time-scale differences between far-ultraviolet – far-infrared and radio-derived star formation rate (SFR) tracers. We examine how the spectral energy distribution (SED)-derived star formation histories (SFHs) of galaxies can be used to explain discrepancies in these SFR tracers, which are sensitive to different time-scales. Galaxies exhibiting an increasing SFH have systematically higher L TIR and SED-derived SFRs than predicted from their 1.4 GHz radio luminosity. This indicates that insufficient time has passed for subsequent supernovae-driven radio emission to accumulate. We show that backtracking the SFR(t) of galaxies along their SED-derived SFHs to a time several hundred megayears prior to their observed epoch will both linearize the SFR– |$L_\mathrm{1.4\, GHz}$| relation and reduce the overall scatter. The minimum scatter in the SFR(t)– |$L_\mathrm{1.4\, GHz}$| is reached at 200 – 300 Myr prior, consistent with theoretical predictions for the time-scales required to disperse the cosmic ray electrons responsible for the synchrotron emission. [ABSTRACT FROM AUTHOR]

Published
2024
Full Text
View/download PDF

4. EPOCHS IX. When cosmic dawn breaks: evidence for evolved stellar populations in 7 < z < 12 galaxies from PEARLS GTO and public NIRCam imaging.

Author

Trussler, James A A, Conselice, Christopher J, Adams, Nathan, Austin, Duncan, Ferreira, Leonardo, Harvey, Tom, Li, Qiong, Vijayan, Aswin P, Wilkins, Stephen M, Windhorst, Rogier A, Bhatawdekar, Rachana, Cheng, Cheng, Coe, Dan, Cohen, Seth H, Driver, Simon P, Frye, Brenda, Grogin, Norman A, Hathi, Nimish, Jansen, Rolf A, and Koekemoer, Anton

Subjects
STELLAR populations, GALAXIES, MID-infrared spectroscopy, SPECTRAL energy distribution, STARS
Abstract

The presence of evolved stars in high-redshift galaxies can place valuable indirect constraints on the onset of star formation in the Universe. Thus, we use PEARLS GTO (Prime Extragalactic Areas for Reionization and Lensing Science Guaranteed Time Observations) and public NIRCam (Near Infrared Camera) photometric data to search for Balmer-break candidate galaxies at 7 < z < 12. We find that our Balmer-break candidates at z ∼ 10.5 tend to be older (115 Myr), have lower inferred [O  iii ] + Hβ equivalent widths (120 Å), have lower specific star formation rates (6 Gyr−1) and redder UV slopes (β = −1.8) than our control sample of galaxies. However, these trends all become less strong at z ∼ 8, where the F 444 W filter now probes the strong rest-frame optical emission lines, thus providing additional constraints on the current star formation activity of these galaxies. Indeed, the bursty nature of epoch of reionization galaxies can lead to a disconnect between their current spectral energy distribution (SED) profiles and their more extended star formation histories. We discuss how strong emission lines, the cumulative effect of weak emission lines, dusty continua, and active galactic nuclei can all contribute to the photometric excess seen in the rest-frame optical, thus mimicking the signature of a Balmer break. Additional medium-band imaging will thus be essential to more robustly identify Balmer-break galaxies. However, the Balmer break alone cannot serve as a definitive proxy for the stellar age of galaxies, being complexly dependent on the star formation history. Ultimately, deep Near Infrared Spectrograph (NIRSpec) continuum spectroscopy and Mid-Infrared Instrument (MIRI) imaging will provide the strongest indirect constraints on the formation era of the first galaxies in the Universe, thereby revealing when cosmic dawn breaks. [ABSTRACT FROM AUTHOR]

Published
2024
Full Text
View/download PDF

5. EPOCHS VII: Discovery of high redshift (6.5 &lt; z &lt; 12) AGN candidates in JWST ERO and PEARLS data

Author

Juodžbalis, Ignas, primary, Conselice, Christopher J, additional, Singh, Maitrayee, additional, Adams, Nathan, additional, Ormerod, Katherine, additional, Harvey, Thomas, additional, Austin, Duncan, additional, Volonteri, Marta, additional, Cohen, Seth H, additional, Jansen, Rolf A, additional, Summers, Jake, additional, Windhorst, Rogier A, additional, D’Silva, Jordan C J, additional, Koekemoer, Anton M, additional, Coe, Dan, additional, Driver, Simon P, additional, Frye, Brenda, additional, Grogin, Norman A, additional, Marshall, Madeline A, additional, Nonino, Mario, additional, Pirzkal, Nor, additional, Robotham, Aaron, additional, Jr, Russell E Ryan, additional, Ortiz, Rafael, additional, Tompkins, Scott, additional, Willmer, Christopher N A, additional, and Yan, Haojing, additional

Published
2023
Full Text
View/download PDF

6. GAMA/DEVILS: cosmic star formation and AGN activity over 12.5 billion years

Author

D’Silva, Jordan C J, primary, Driver, Simon P, additional, Lagos, Claudia D P, additional, Robotham, Aaron S G, additional, Bellstedt, Sabine, additional, Davies, Luke J M, additional, Thorne, Jessica E, additional, Bland-Hawthorn, Joss, additional, Bravo, Matias, additional, Holwerda, Benne, additional, Phillipps, Steven, additional, Seymour, Nick, additional, Siudek, Malgorzata, additional, and Windhorst, Rogier A, additional

Published
2023
Full Text
View/download PDF

7. Galaxy And Mass Assembly (GAMA): The group H i mass as a function of halo mass

Author

Dev, Ajay, primary, Driver, Simon P, additional, Meyer, Martin, additional, Roychowdhury, Sambit, additional, Rhee, Jonghwan, additional, Stevens, Adam R H, additional, Claudia del Lagos, P, additional, Bland-Hawthorn, Joss, additional, Catinella, Barbara, additional, Hopkins, A M, additional, Loveday, Jonathan, additional, Obreschkow, Danail, additional, Phillipps, Steven, additional, and Robotham, Aaron S G, additional

Published
2023
Full Text
View/download PDF

8. JWST’s PEARLS: TN J1338–1942 – I. Extreme jet-triggered star formation in a z = 4.11 luminous radio galaxy

Author

Duncan, Kenneth J, primary, Windhorst, Rogier A, additional, Koekemoer, Anton M, additional, Röttgering, Huub J A, additional, Cohen, Seth H, additional, Jansen, Rolf A, additional, Summers, Jake, additional, Tompkins, Scott, additional, Hutchison, Taylor A, additional, Conselice, Christopher J, additional, Driver, Simon P, additional, Yan, Haojing, additional, Adams, Nathan J, additional, Cheng, Cheng, additional, Coe, Dan, additional, Diego, Jose M, additional, Dole, Hervé, additional, Frye, Brenda, additional, Gim, Hansung B, additional, Grogin, Norman A, additional, Holwerda, Benne W, additional, Lim, Jeremy, additional, Marshall, Madeline A, additional, Nonino, Mario, additional, Pirzkal, Nor, additional, Robotham, Aaron, additional, Ryan, Russell E, additional, and Willmer, Christopher N A, additional

Published
2023
Full Text
View/download PDF

9. EPOCHS VII: discovery of high-redshift (6.5 < z < 12) AGN candidates in JWST ERO and PEARLS data.

Author

Juodžbalis, Ignas, Conselice, Christopher J, Singh, Maitrayee, Adams, Nathan, Ormerod, Katherine, Harvey, Thomas, Austin, Duncan, Volonteri, Marta, Cohen, Seth H, Jansen, Rolf A, Summers, Jake, Windhorst, Rogier A, D'Silva, Jordan C J, Koekemoer, Anton M, Coe, Dan, Driver, Simon P, Frye, Brenda, Grogin, Norman A, Marshall, Madeline A, and Nonino, Mario

Subjects
GALACTIC redshift, SPECTRAL energy distribution, BLACK holes, SUPERMASSIVE black holes, DETECTION limit, REDSHIFT
Abstract

We present an analysis of a sample of robust high-redshift galaxies selected from the 'blank' fields of the Prime Extragalactic Areas for Reionization Science (PEARLS) survey and Early Release Observations (ERO) data from JWST with the aim of selecting candidate high-redshift active galactic nuclei (AGN). Sources were identified from this parent sample using a threefold selection procedure, which includes spectral energy distribution (SED) fitting to identify sources that are best fitted by AGN SED templates, a further selection based on the relative performance of AGN and non-AGN models, and finally morphological fitting to identify compact sources of emission, resulting in a purity-oriented procedure. Using this procedure, we identify a sample of nine AGN candidates at 6.5 < z < 12, from which we constrain their physical properties as well as measure a lower bound on the AGN fraction in this redshift range of 5 ± 1 per cent. As this is an extreme lower limit due to our focus on purity and our SEDs being calibrated for unobscured Type 1 AGN, this demonstrates that AGN are perhaps quite common at this early epoch. The rest-frame UV colours of our candidate objects suggest that these systems are potentially candidate obese black hole galaxies (OBGs). We also investigate Chandra and VLA maps of these areas from which we calculate detection limits. Of note is a z  = 11.9 candidate source exhibiting an abrupt morphological shift in the reddest band as compared to bluer bands, indicating a potential merger or an unusually strong outflow. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

10. GAMA/DEVILS: cosmic star formation and AGN activity over 12.5 billion years.

Author

D'Silva, Jordan C J, Driver, Simon P, Lagos, Claudia D P, Robotham, Aaron S G, Bellstedt, Sabine, Davies, Luke J M, Thorne, Jessica E, Bland-Hawthorn, Joss, Bravo, Matias, Holwerda, Benne, Phillipps, Steven, Seymour, Nick, Siudek, Malgorzata, and Windhorst, Rogier A

Subjects
*STAR formation, *ACTIVE galactic nuclei, *SPECTRAL energy distribution, *STELLAR mass, *LIFE cycles (Biology), *STELLAR activity
Abstract

We use the Galaxy and Mass Assembly (GAMA) and the Deep Extragalactic Visible Legacy Survey (DEVILS) observational data sets to calculate the cosmic star formation rate (SFR) and active galactic nuclei (AGN) bolometric luminosity history (CSFH/CAGNH) over the last 12.5 billion years. SFRs and AGN bolometric luminosities were derived using the spectral energy distribution fitting code ProSpect , which includes an AGN prescription to self-consistently model the contribution from both AGN and stellar emission to the observed rest-frame ultra-violet to far-infrared photometry. We find that both the CSFH and CAGNH evolve similarly, rising in the early Universe up to a peak at look-back time ≈10 Gyr (z ≈ 2), before declining towards the present day. The key result of this work is that we find the ratio of CAGNH to CSFH has been flat (⁠|$\approx 10^{42.5}\, \mathrm{erg \, s^{-1}\, {\rm M}_{\odot }^{-1}\, yr}$|⁠) for 11 Gyr up to the present day, indicating that star formation and AGN activity have been coeval over this time period. We find that the stellar masses of the galaxies that contribute most to the CSFH and CAGNH are similar, implying a common cause, which is likely gas inflow. The depletion of the gas supply suppresses cosmic star formation and AGN activity equivalently to ensure that they have experienced similar declines over the last 10 Gyr. These results are an important milestone for reconciling the role of star formation and AGN activity in the life cycle of galaxies. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

13. The cosmic radio background from 150 MHz to 8.4 GHz and its division into AGN and star-forming galaxy flux.

Author

Tompkins, Scott A, Driver, Simon P, Robotham, Aaron S G, Windhorst, Rogier A, Lagos, Claudia del P, Vernstrom, T, and Hopkins, Andrew M

Subjects
*SPECTRAL energy distribution, *ACTIVE galactic nuclei, *COSMIC background radiation, *RADIO sources (Astronomy), *NUCLEAR astrophysics, *RADIO frequency
Abstract

We present a revised measurement of the extragalactic background light (EBL) at radio frequencies based on a near complete compendium of radio source counts. We present the radio-EBL at 150 MHz, 325 MHz, 610 MHz, 1.4 GHz, 3 GHz, 5 GHz, and 8.4 GHz. In all cases the contribution to the radio-EBL, per decade of flux, exhibits a two-humped distribution well matched to the active galactic nucleus (AGN) and star-forming galaxy (SFG) populations, and with each population contributing roughly equal energy. Only at 3 GHz are the source count contributions to the EBL fully convergent, and hence we report empirical lower limits to the radio-EBL in the remaining bands. Adopting predictions from the SHARK semi-analytic model for the form of the SFG population, we can fit the fainter source counts providing measurements of the total contribution to the radio-EBL for the SFG and the AGN populations separately. This constitutes an empirically constrained model-dependent measurement for the SFG contribution, but a fully empirical measurement of the AGN contribution. Using the ProSpect spectral energy distribution code we can model the ultraviolet-optical-infrared-mm-radio SFG EBL at all frequencies from the cosmic star-formation history and the adoption of a Chabrier initial mass function. However, significant discrepancy remains (5 ×) between our source-count estimates of the radio-EBL and the direct measurements reported from the Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission-2 (ARCADE-2) experiment. We can rule out a significant missing discrete source radio population and suggest that the cause of the high ARCADE-2 radio-EBL values may need to be sought either in the foreground subtraction or as a yet unknown diffuse component in the radio sky. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

14. Deep investigation of neutral gas origins (DINGO): H i stacking experiments with early science data

Author

Rhee, Jonghwan, primary, Meyer, Martin, additional, Popping, Attila, additional, Bellstedt, Sabine, additional, Driver, Simon P, additional, Robotham, Aaron S G, additional, Whiting, Matthew, additional, Baldry, Ivan K, additional, Brough, Sarah, additional, Brown, Michael J I, additional, Bunton, John D, additional, Dodson, Richard, additional, Holwerda, Benne W, additional, Hopkins, Andrew M, additional, Koribalski, Bärbel S, additional, Lee-Waddell, Karen, additional, López-Sánchez, Ángel R, additional, Loveday, Jon, additional, Mahony, Elizabeth, additional, Roychowdhury, Sambit, additional, Rozgonyi, Kristóf, additional, and Staveley-Smith, Lister, additional

Published
2022
Full Text
View/download PDF

15. Galaxy And Mass Assembly (GAMA): bulge-disc decomposition of KiDS data in the nearby Universe

Author

Casura, Sarah, primary, Liske, Jochen, additional, Robotham, Aaron S G, additional, Brough, Sarah, additional, Driver, Simon P, additional, Graham, Alister W, additional, Häußler, Boris, additional, Holwerda, Benne W, additional, Hopkins, Andrew M, additional, Kelvin, Lee S, additional, Moffett, Amanda J, additional, Taranu, Dan S, additional, and Taylor, Edward N, additional

Published
2022
Full Text
View/download PDF

16. Deep extragalactic visible legacy survey (DEVILS): the emergence of bulges and decline of disc growth since z = 1

Author

Hashemizadeh, Abdolhosein, primary, Driver, Simon P, additional, Davies, Luke J M, additional, Robotham, Aaron S G, additional, Bellstedt, Sabine, additional, Foster, Caroline, additional, Holwerda, Benne W, additional, Jarvis, Matt, additional, Phillipps, Steven, additional, Siudek, Malgorzata, additional, Thorne, Jessica E, additional, Windhorst, Rogier A, additional, and Wolf, Christian, additional

Published
2022
Full Text
View/download PDF

17. An empirical measurement of the halo mass function from the combination of GAMA DR4, SDSS DR12, and REFLEX II data

Author

Driver, Simon P, primary, Robotham, Aaron S G, additional, Obreschkow, Danail, additional, Peacock, John A, additional, Baldry, Ivan K, additional, Bellstedt, Sabine, additional, Bland-Hawthorn, Joss, additional, Brough, Sarah, additional, Cluver, Michelle, additional, Holwerda, Benne W, additional, Hopkins, Andrew, additional, Lagos, Claudia, additional, Liske, Jochen, additional, Loveday, Jon, additional, Phillipps, Steven, additional, and Taylor, Edward N, additional

Published
2022
Full Text
View/download PDF

18. The LEGA-C and SAMI galaxy surveys: quiescent stellar populations and the mass–size plane across 6 Gyr

Author

Barone, Tania M, primary, D’Eugenio, Francesco, additional, Scott, Nicholas, additional, Colless, Matthew, additional, Vaughan, Sam P, additional, van der Wel, Arjen, additional, Fraser-McKelvie, Amelia, additional, de Graaff, Anna, additional, van de Sande, Jesse, additional, Wu(吳柏鋒), Po-Feng, additional, Bezanson, Rachel, additional, Brough, Sarah, additional, Bell, Eric, additional, Croom, Scott M, additional, Cortese, Luca, additional, Driver, Simon, additional, Gallazzi, Anna R, additional, Muzzin, Adam, additional, Sobral, David, additional, Bland-Hawthorn, Joss, additional, Bryant, Julia J, additional, Goodwin, Michael, additional, Lawrence, Jon S, additional, Lorente, Nuria P F, additional, and Owers, Matt S, additional

Published
2022
Full Text
View/download PDF

19. Galaxy And Mass Assembly (GAMA): Data Release 4 and the z &lt; 0.1 total and z &lt; 0.08 morphological galaxy stellar mass functions

Author

Driver, Simon P, primary, Bellstedt, Sabine, additional, Robotham, Aaron S G, additional, Baldry, Ivan K, additional, Davies, Luke J, additional, Liske, Jochen, additional, Obreschkow, Danail, additional, Taylor, Edward N, additional, Wright, Angus H, additional, Alpaslan, Mehmet, additional, Bamford, Steven P, additional, Bauer, Amanda E, additional, Bland-Hawthorn, Joss, additional, Bilicki, Maciej, additional, Bravo, Matías, additional, Brough, Sarah, additional, Casura, Sarah, additional, Cluver, Michelle E, additional, Colless, Matthew, additional, Conselice, Christopher J, additional, Croom, Scott M, additional, de Jong, Jelte, additional, D’Eugenio, Franceso, additional, De Propris, Roberto, additional, Dogruel, Burak, additional, Drinkwater, Michael J, additional, Dvornik, Andrej, additional, Farrow, Daniel J, additional, Frenk, Carlos S, additional, Giblin, Benjamin, additional, Graham, Alister W, additional, Grootes, Meiert W, additional, Gunawardhana, Madusha L P, additional, Hashemizadeh, Abdolhosein, additional, Häußler, Boris, additional, Heymans, Catherine, additional, Hildebrandt, Hendrik, additional, Holwerda, Benne W, additional, Hopkins, Andrew M, additional, Jarrett, Tom H, additional, Heath Jones, D, additional, Kelvin, Lee S, additional, Koushan, Soheil, additional, Kuijken, Konrad, additional, Lara-López, Maritza A, additional, Lange, Rebecca, additional, López-Sánchez, Ángel R, additional, Loveday, Jon, additional, Mahajan, Smriti, additional, Meyer, Martin, additional, Moffett, Amanda J, additional, Napolitano, Nicola R, additional, Norberg, Peder, additional, Owers, Matt S, additional, Radovich, Mario, additional, Raouf, Mojtaba, additional, Peacock, John A, additional, Phillipps, Steven, additional, Pimbblet, Kevin A, additional, Popescu, Cristina, additional, Said, Khaled, additional, Sansom, Anne E, additional, Seibert, Mark, additional, Sutherland, Will J, additional, Thorne, Jessica E, additional, Tuffs, Richard J, additional, Turner, Ryan, additional, van der Wel, Arjen, additional, van Kampen, Eelco, additional, and Wilkins, Steve M, additional

Published
2022
Full Text
View/download PDF

20. Deep investigation of neutral gas origins (DINGO): H i stacking experiments with early science data.

Author

Rhee, Jonghwan, Meyer, Martin, Popping, Attila, Bellstedt, Sabine, Driver, Simon P, Robotham, Aaron S G, Whiting, Matthew, Baldry, Ivan K, Brough, Sarah, Brown, Michael J I, Bunton, John D, Dodson, Richard, Holwerda, Benne W, Hopkins, Andrew M, Koribalski, Bärbel S, Lee-Waddell, Karen, López-Sánchez, Ángel R, Loveday, Jon, Mahony, Elizabeth, and Roychowdhury, Sambit

Subjects
DINGO, STELLAR density (Stellar population), DATA science, GALAXY clusters, SCIENTIFIC experimentation, STELLAR mass
Abstract

We present early science results from Deep Investigation of Neutral Gas Origins (DINGO), an |$\rm H$| i survey using the Australian Square Kilometre Array Pathfinder (ASKAP). Using ASKAP subarrays available during its commissioning phase, DINGO early science data were taken over ∼60 deg2 of the Galaxy And Mass Assembly (GAMA) 23 h region with 35.5 h integration time. We make direct detections of six known and one new sources at z < 0.01. Using |$\rm H$|   i spectral stacking, we investigate the |$\rm H$|   i gas content of galaxies at 0.04 < z < 0.09 for different galaxy colours. The results show that galaxy morphology based on optical colour is strongly linked to |$\rm H$|   i gas properties. To examine environmental impacts on the |$\rm H$| i gas content of galaxies, three subsamples are made based on the GAMA group catalogue. The average |$\rm H$| i mass of group central galaxies is larger than those of satellite and isolated galaxies, but with a lower |$\rm H$| i gas fraction. We derive a variety of |$\rm H$| i scaling relations for physical properties of our sample, including stellar mass, stellar mass surface density, NUV − r colour, specific star formation rate, and halo mass. We find that the derived |$\rm H$| i scaling relations are comparable to other published results, with consistent trends also observed to ∼0.5 dex lower limits in stellar mass and stellar surface density. The cosmic |$\rm H$| i densities derived from our data are consistent with other published values at similar redshifts. DINGO early science highlights the power of |$\rm H$| i spectral stacking techniques with ASKAP. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

21. Galaxy And Mass Assembly (GAMA): extended intragroup light in a group at z = 0.2 from deep Hyper Suprime-Cam images.

Author

Martínez-Lombilla, Cristina, Brough, Sarah, Montes, Mireia, Baena-Gallé, Roberto, Akhlaghi, Mohammad, Infante-Sainz, Raúl, Driver, Simon P, Holwerda, Benne W, Pimbblet, Kevin A, and Robotham, Aaron S G

Subjects
GALAXY clusters, GALAXIES, DATA release, STELLAR populations, IMAGE analysis
Abstract

We present a pilot study to assess the potential of Hyper Suprime-Cam Public Data Release 2 (HSC-PDR2) images for the analysis of extended faint structures within groups of galaxies. We examine the intragroup light (IGL) of the group 400138 (M dyn = 1.3 ± 0.5 × 1013 M⊙, z ∼ 0.2) from the Galaxy And Mass Assembly (GAMA) survey using Hyper Suprime-Cam Subaru Strategic Program Public Data Release 2 (HSC-SSP PDR2) images in g, r , and i bands. We present the most extended IGL measurement to date, reaching down to |$\mu _{g}^{\rm {lim}}=30.76$|  mag arcsec−2 (3σ; 10 × 10 arcsec2) at a semimajor axis of 275 kpc. The IGL shows mean colour values of g − i  = 0.92, g − r  = 0.60, and r − i  = 0.32 (±0.01). The IGL stellar populations are younger (2–2.5 Gyr) and less metal rich ([Fe/H] ∼ −0.4) than those of the host group galaxies. We find a range of IGL fractions as a function of total group luminosity of |${\sim} 2\!-\!36 {{\ \rm per\ cent}}$| depending on the definition of IGL, with larger fractions the bluer the observation wavelength. The early-type to late-type galaxy ratio suggests that 400138 is a more evolved group, dominated by early-type galaxies, and the IGL fraction agrees with that of other similarly evolved groups. These results are consistent with tidal stripping of the outer parts of Milky Way-like galaxies as the main driver of the IGL build-up. This is supported by the detection of substructure in the IGL towards the galaxy member 1660615 suggesting a recent interaction (<1 Gyr ago) of that galaxy with the core of the group. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

22. Deep Extragalactic VIsible Legacy Survey (DEVILS): identification of AGN through SED fitting and the evolution of the bolometric AGN luminosity function

Author

Thorne, Jessica E, primary, Robotham, Aaron S G, additional, Davies, Luke J M, additional, Bellstedt, Sabine, additional, Brown, Michael J I, additional, Croom, Scott M, additional, Delvecchio, Ivan, additional, Groves, Brent, additional, Jarvis, Matt J, additional, Shabala, Stanislav S, additional, Seymour, Nick, additional, Whittam, Imogen H, additional, Bravo, Matias, additional, Cook, Robin H W, additional, Driver, Simon P, additional, Holwerda, Benne, additional, Phillipps, Steven, additional, and Siudek, Malgorzata, additional

Published
2021
Full Text
View/download PDF

23. Galaxy And Mass Assembly (GAMA): z ~ 0 galaxy luminosity function down to L ~ 106 L⊙ via clustering based redshift inference

Author

Karademir, Geray S, primary, Taylor, Edward N, additional, Blake, Chris, additional, Baldry, Ivan K, additional, Bellstedt, Sabine, additional, Bilicki, Maciej, additional, Brown, Michael J I, additional, Cluver, Michelle E, additional, Driver, Simon P, additional, Hildebrandt, Hendrik, additional, Holwerda, Benne W, additional, Hopkins, Andrew M, additional, Loveday, Jonathan, additional, Phillipps, Steven, additional, and Wright, Angus H, additional

Published
2021
Full Text
View/download PDF

24. Measuring cosmic density of neutral hydrogen via stacking the DINGO-VLA data

Author

Chen, Qingxiang, primary, Meyer, Martin, additional, Popping, Attila, additional, Staveley-Smith, Lister, additional, Bryant, Julia, additional, Delhaize, Jacinta, additional, Holwerda, B W, additional, Cluver, M E, additional, Loveday, J, additional, Lopez-Sanchez, Angel R, additional, Zwaan, Martin, additional, Taylor, E N, additional, Hopkins, A M, additional, Wright, Angus, additional, Driver, Simon, additional, and Brough, S, additional

Published
2021
Full Text
View/download PDF

25. empirical measurement of the halo mass function from the combination of GAMA DR4, SDSS DR12, and REFLEX II data.

Author

Driver, Simon P, Robotham, Aaron S G, Obreschkow, Danail, Peacock, John A, Baldry, Ivan K, Bellstedt, Sabine, Bland-Hawthorn, Joss, Brough, Sarah, Cluver, Michelle, Holwerda, Benne W, Hopkins, Andrew, Lagos, Claudia, Liske, Jochen, Loveday, Jon, Phillipps, Steven, and Taylor, Edward N

Subjects
*MASS measurement, *DARK matter, *GALAXY clusters, *ASTRONOMICAL surveys, *X-ray binaries, *REFLEXES
Abstract

We construct the halo mass function (HMF) from the GAMA (Galaxy And Mass Assembly) galaxy group catalogue over the mass range of 1012.7–1015.5 M⊙, and find good agreement with the expectation from Lambda cold dark matter. In comparison to previous studies, this result extends the mass range over which the HMF has now been measured over by an order of magnitude. We combine the GAMA data release (DR) 4 HMF with similar data from the Sloan Digital Sky Survey (SDSS) DR12 and REFLEX II (ROSAT -ESO Flux Limited X-ray Galaxy Cluster Survey) surveys, and fit a four-parameter Murray–Robotham–Power function, valid at |$\tilde{z} \approx 0.1$|⁠ , yielding a density normalization of log10 (ϕ* Mpc |$^{3})= -3.96^{+0.55}_{-0.82}$|⁠ , a high mass turnover of log10 (M * M |$_{\odot }^{-1})=14.13^{+0.43}_{-0.40}$|⁠ , a low-mass power-law slope of |$\alpha =-1.68^{+0.21}_{-0.24}$|⁠ , and a high-mass softening parameter of |$\beta =0.63^{+0.25}_{-0.11}$|⁠. If we fold in the constraint on ΩM from the Planck 2018 cosmology, we are able to reduce these uncertainties further, but this relies on the assumption that the power-law trend can be extrapolated from 1012.7 M⊙ to zero mass. Throughout, we highlight the effort needed to improve on our HMF measurement: improved halo mass estimates that do not rely on calibration to simulations; reduced halo mass uncertainties needed to mitigate the strong Eddington bias that arises from the steepness of the HMF low-mass slope; and deeper wider area spectroscopic surveys. To our halo mass limit of 1012.7 M⊙, we are directly resolving ('seeing') 41 ± 5 per cent of the total mass density, i.e. ΩM,>12.7 = 0.128 ± 0.016, opening the door for the direct construction of three-dimensional dark matter mass maps at Mpc resolution. [ABSTRACT FROM AUTHOR]

Published
2022
Full Text
View/download PDF

26. Deep Extragalactic VIsible Legacy Survey (DEVILS): SED fitting in the D10-COSMOS field and the evolution of the stellar mass function and SFR–M⋆ relation

Author

Thorne, Jessica E, primary, Robotham, Aaron S G, additional, Davies, Luke J M, additional, Bellstedt, Sabine, additional, Driver, Simon P, additional, Bravo, Matías, additional, Bremer, Malcolm N, additional, Holwerda, Benne W, additional, Hopkins, Andrew M, additional, Lagos, Claudia del P, additional, Phillipps, Steven, additional, Siudek, Malgorzata, additional, Taylor, Edward N, additional, and Wright, Angus H, additional

Published
2021
Full Text
View/download PDF

27. Galaxy And Mass Assembly (GAMA): Data Release 4 and the z < 0.1 total and z < 0.08 morphological galaxy stellar mass functions.

Author

Driver, Simon P, Bellstedt, Sabine, Robotham, Aaron S G, Baldry, Ivan K, Davies, Luke J, Liske, Jochen, Obreschkow, Danail, Taylor, Edward N, Wright, Angus H, Alpaslan, Mehmet, Bamford, Steven P, Bauer, Amanda E, Bland-Hawthorn, Joss, Bilicki, Maciej, Bravo, Matías, Brough, Sarah, Casura, Sarah, Cluver, Michelle E, Colless, Matthew, and Conselice, Christopher J

Subjects
*STELLAR mass, *DATA release, *STELLAR density (Stellar population), *GALAXY spectra, *GALAXY clusters, *GALAXY mergers
Abstract

In Galaxy And Mass Assembly Data Release 4 (GAMA DR4), we make available our full spectroscopic redshift sample. This includes 248 682 galaxy spectra, and, in combination with earlier surveys, results in 330 542 redshifts across five sky regions covering ∼250 deg2. The redshift density, is the highest available over such a sustained area, has exceptionally high completeness (95 per cent to r KiDS = 19.65 mag), and is well-suited for the study of galaxy mergers, galaxy groups, and the low redshift (z  < 0.25) galaxy population. DR4 includes 32 value-added tables or Data Management Units (DMUs) that provide a number of measured and derived data products including GALEX , ESO KiDS, ESO VIKING, WISE , and Herschel Space Observatory imaging. Within this release, we provide visual morphologies for 15 330 galaxies to z  < 0.08, photometric redshift estimates for all 18 million objects to r KiDS ∼ 25 mag, and stellar velocity dispersions for 111 830 galaxies. We conclude by deriving the total galaxy stellar mass function (GSMF) and its sub-division by morphological class (elliptical, compact-bulge and disc, diffuse-bulge and disc, and disc only). This extends our previous measurement of the total GSMF down to 106.75 M |$_{\odot } \, h_{70}^{-2}$| and we find a total stellar mass density of ρ * = (2.97 ± 0.04) × 108 M |$_{\odot } \, h_{70}$|  Mpc−3 or |$\Omega _*=(2.17 \pm 0.03) \times 10^{-3} \, h_{70}^{-1}$|⁠. We conclude that at z  < 0.1, the Universe has converted 4.9 ± 0.1 per cent of the baryonic mass implied by big bang Nucleosynthesis into stars that are gravitationally bound within the galaxy population. [ABSTRACT FROM AUTHOR]

Published
2022
Full Text
View/download PDF

28. LEGA-C and SAMI galaxy surveys: quiescent stellar populations and the mass–size plane across 6 Gyr.

Author

Barone, Tania M, D'Eugenio, Francesco, Scott, Nicholas, Colless, Matthew, Vaughan, Sam P, van der Wel, Arjen, Fraser-McKelvie, Amelia, de Graaff, Anna, van de Sande, Jesse, Wu(吳柏鋒), Po-Feng, Bezanson, Rachel, Brough, Sarah, Bell, Eric, Croom, Scott M, Cortese, Luca, Driver, Simon, Gallazzi, Anna R, Muzzin, Adam, Sobral, David, and Bland-Hawthorn, Joss

Subjects
STELLAR populations, VIRIAL theorem, GRAVITATIONAL potential, GALAXIES, STELLAR mass, REDSHIFT
Abstract

We investigate changes in stellar population age and metallicity ([Z/H]) scaling relations for quiescent galaxies from intermediate redshift (0.60 ≤   |$z$| ≤ 0.76) using the LEGA-C Survey to low redshift (0.014 ≤   |$z$| ≤ 0.10) using the SAMI Galaxy Survey. Specifically, we study how the spatially integrated global age and metallicity of individual quiescent galaxies vary in the mass–size plane, using the stellar mass M * and a dynamical mass proxy derived from the virial theorem M D  ∝ σ2  R e. We find that, similarly to at low redshift, the metallicity of quiescent galaxies at 0.60 ≤   |$z$| ≤ 0.76 closely correlates with M / R e (a proxy for the gravitational potential or escape velocity), in that galaxies with deeper potential wells are more metal-rich. This supports the hypothesis that the relation arises due to the gravitational potential regulating the retention of metals by determining the escape velocity for metal-rich stellar and supernova ejecta to escape the system and avoid being recycled into later stellar generations. Conversely, we find no correlation between age and surface density (⁠|$M/R_\mathrm{e}^2$|⁠) at 0.60 ≤   |$z$| ≤ 0.76, despite this relation being strong at low redshift. We consider this change in the age– |$M/R_\mathrm{e}^2$| relation in the context of the redshift evolution of the star-forming and quiescent mass–size relations, and find our results are consistent with galaxies forming more compactly at higher redshifts and remaining compact throughout their evolution. Furthermore, galaxies appear to quench at a characteristic surface density that decreases with decreasing redshift. The |$z$| ∼  0 age– |$M/R_\mathrm{e}^2$| relation is therefore a result of building up the quiescent and star-forming populations with galaxies that formed at a range of redshifts and therefore a range of surface densities. [ABSTRACT FROM AUTHOR]

Published
2022
Full Text
View/download PDF

29. Deep extragalactic visible legacy survey (DEVILS): stellar mass growth by morphological type since z = 1

Author

Hashemizadeh, Abdolhosein, primary, Driver, Simon P, additional, Davies, Luke J M, additional, Robotham, Aaron S G, additional, Bellstedt, Sabine, additional, Windhorst, Rogier A, additional, Bremer, Malcolm, additional, Phillipps, Steven, additional, Jarvis, Matt, additional, Holwerda, Benne W, additional, Lagos, Claudia del P, additional, Koushan, Soheil, additional, Siudek, Malgorzata, additional, Maddox, Natasha, additional, Thorne, Jessica E, additional, and Elahi, Pascal, additional

Published
2021
Full Text
View/download PDF

31. GAMA/DEVILS: constraining the cosmic star formation history from improved measurements of the 0.3–2.2 μm extragalactic background light

Author

Koushan, Soheil, primary, Driver, Simon P, additional, Bellstedt, Sabine, additional, Davies, Luke J, additional, Robotham, Aaron S G, additional, Lagos, Claudia del P, additional, Hashemizadeh, Abdolhosein, additional, Obreschkow, Danail, additional, Thorne, Jessica E, additional, Bremer, Malcolm, additional, Holwerda, B W, additional, Hopkins, Andrew M, additional, Jarvis, Matt J, additional, Siudek, Malgorzata, additional, and Windhorst, Rogier A, additional

Published
2021
Full Text
View/download PDF

32. The SAMI Galaxy Survey: the third and final data release

Author

Croom, Scott M, primary, Owers, Matt S, additional, Scott, Nicholas, additional, Poetrodjojo, Henry, additional, Groves, Brent, additional, van de Sande, Jesse, additional, Barone, Tania M, additional, Cortese, Luca, additional, D’Eugenio, Francesco, additional, Bland-Hawthorn, Joss, additional, Bryant, Julia, additional, Oh, Sree, additional, Brough, Sarah, additional, Agostino, James, additional, Casura, Sarah, additional, Catinella, Barbara, additional, Colless, Matthew, additional, Cecil, Gerald, additional, Davies, Roger L, additional, Drinkwater, Michael J, additional, Driver, Simon P, additional, Ferreras, Ignacio, additional, Foster, Caroline, additional, Fraser-McKelvie, Amelia, additional, Lawrence, Jon, additional, Leslie, Sarah K, additional, Liske, Jochen, additional, López-Sánchez, Ángel R, additional, Lorente, Nuria P F, additional, McElroy, Rebecca, additional, Medling, Anne M, additional, Obreschkow, Danail, additional, Richards, Samuel N, additional, Sharp, Rob, additional, Sweet, Sarah M, additional, Taranu, Dan S, additional, Taylor, Edward N, additional, Tescari, Edoardo, additional, Thomas, Adam D, additional, Tocknell, James, additional, and Vaughan, Sam P, additional

Published
2021
Full Text
View/download PDF

33. Galaxy And Mass Assembly (GAMA): a forensic SED reconstruction of the cosmic star formation history and metallicity evolution by galaxy type

Author

Bellstedt, Sabine, primary, Robotham, Aaron S G, additional, Driver, Simon P, additional, Thorne, Jessica E, additional, Davies, Luke J M, additional, Lagos, Claudia del P, additional, Stevens, Adam R H, additional, Taylor, Edward N, additional, Baldry, Ivan K, additional, Moffett, Amanda J, additional, Hopkins, Andrew M, additional, and Phillipps, Steven, additional

Published
2020
Full Text
View/download PDF

34. Galaxy And Mass Assembly (GAMA): assimilation of KiDS into the GAMA database

Author

Bellstedt, Sabine, primary, Driver, Simon P, additional, Robotham, Aaron S G, additional, Davies, Luke J M, additional, Bogue, Kamran R J, additional, Cook, Robin H W, additional, Hashemizadeh, Abdolhosein, additional, Koushan, Soheil, additional, Taylor, Edward N, additional, Thorne, Jessica E, additional, Turner, Ryan J, additional, and Wright, Angus H, additional

Published
2020
Full Text
View/download PDF

35. From the far-ultraviolet to the far-infrared – galaxy emission at 0 ≤ z ≤ 10 in the shark semi-analytic model

Author

Lagos, Claudia del P, primary, Robotham, Aaron S G, additional, Trayford, James W, additional, Tobar, Rodrigo, additional, Bravo, Matías, additional, Bellstedt, Sabine, additional, Davies, Luke J M, additional, Driver, Simon P, additional, Elahi, Pascal J, additional, Obreschkow, Danail, additional, and Power, Chris, additional

Published
2019
Full Text
View/download PDF

36. Star-forming, rotating spheroidal galaxies in the GAMA and SAMI surveys

Author

Moffett, Amanda J, primary, Phillipps, Steven, additional, Robotham, Aaron S G, additional, Driver, Simon P, additional, Bremer, Malcolm N, additional, Cortese, Luca, additional, Wong, O Ivy, additional, Brough, Sarah, additional, Brown, Michael J I, additional, Bryant, Julia J, additional, Conselice, Christopher J, additional, Croom, Scott M, additional, George, Koshy, additional, Goldstein, Greg, additional, Goodwin, Michael, additional, Holwerda, Benne W, additional, Hopkins, Andrew M, additional, Konstantopoulos, Iraklis S, additional, Lawrence, Jon S, additional, Lorente, Nuria P F, additional, Medling, Anne M, additional, Owers, Matt S, additional, Pimbblet, Kevin A, additional, Richards, Samuel N, additional, Sweet, Sarah M, additional, and van de Sande, Jesse, additional

Published
2019
Full Text
View/download PDF

37. Deep Extragalactic VIsible Legacy Survey (DEVILS): SED fitting in the D10-COSMOS field and the evolution of the stellar mass function and SFR–M⋆ relation.

Author

Thorne, Jessica E, Robotham, Aaron S G, Davies, Luke J M, Bellstedt, Sabine, Driver, Simon P, Bravo, Matías, Bremer, Malcolm N, Holwerda, Benne W, Hopkins, Andrew M, Lagos, Claudia del P, Phillipps, Steven, Siudek, Malgorzata, Taylor, Edward N, and Wright, Angus H

Subjects
STELLAR evolution, STELLAR mass, SPECTRAL energy distribution, STELLAR populations, GALACTIC redshift, STAR formation
Abstract

We present catalogues of stellar masses, star formation rates (SFRs), and ancillary stellar population parameters for galaxies spanning 0 < z < 9 from the Deep Extragalactic VIsible Legacy Survey (DEVILS). DEVILS is a deep spectroscopic redshift survey with very high completeness, covering several premier deep fields including COSMOS (D10). Our stellar mass and SFR estimates are self-consistently derived using the spectral energy distribution (SED) modelling code ProSpect , using well-motivated parametrizations for dust attenuation, star formation histories, and metallicity evolution. We show how these improvements, and especially our physically motivated assumptions about metallicity evolution, have an appreciable systematic effect on the inferred stellar masses, at the level of ∼0.2 dex. To illustrate the scientific value of these data, we map the evolving galaxy stellar mass function (SMF) and the SFR– M ⋆ relation for 0 < z < 4.25. In agreement with past studies, we find that most of the evolution in the SMF is driven by the characteristic density parameter, with little evolution in the characteristic mass and low-mass slopes. Where the SFR– M ⋆ relation is indistinguishable from a power law at z > 2.6, we see evidence of a bend in the relation at low redshifts (z < 0.45). This suggests evolution in both the normalization and shape of the SFR– M ⋆ relation since cosmic noon. It is significant that we only clearly see this bend when combining our new DEVILS measurements with consistently derived values for lower redshift galaxies from the Galaxy And Mass Assembly (GAMA) survey: this shows the power of having consistent treatment for galaxies at all redshifts. [ABSTRACT FROM AUTHOR]

Published
2021
Full Text
View/download PDF

38. The SAMI Galaxy Survey: Data Release Two with absorption-line physics value-added products

Author

Scott, Nicholas, primary, van de Sande, Jesse, additional, Croom, Scott M, additional, Groves, Brent, additional, Owers, Matt S, additional, Poetrodjojo, Henry, additional, D’Eugenio, Francesco, additional, Medling, Anne M, additional, Barat, Dilyar, additional, Barone, Tania M, additional, Bland-Hawthorn, Joss, additional, Brough, Sarah, additional, Bryant, Julia, additional, Cortese, Luca, additional, Foster, Caroline, additional, Green, Andrew W, additional, Oh, Sree, additional, Colless, Matthew, additional, Drinkwater, Michael J, additional, Driver, Simon P, additional, Goodwin, Michael, additional, Gunawardhana, Madusha L P, additional, Federrath, Christoph, additional, Harischandra, Lloyd, additional, Jin, Yifei, additional, Lawrence, J S, additional, Lorente, Nuria P, additional, Mannering, Elizabeth, additional, O’Toole, Simon, additional, Richards, Samuel N, additional, Sanchez, Sebastian F, additional, Schaefer, Adam L, additional, Sealey, Katrina, additional, Sharp, Rob, additional, Sweet, Sarah M, additional, Taranu, Dan S, additional, and Varidel, Mathew, additional

Published
2018
Full Text
View/download PDF

39. The causes of the red sequence, the blue cloud, the green valley, and the green mountain

Author

Eales, Stephen A, primary, Baes, Maarten, additional, Bourne, Nathan, additional, Bremer, Malcolm, additional, Brown, Michael J I, additional, Clark, Christopher, additional, Clements, David, additional, de Vis, Pieter, additional, Driver, Simon, additional, Dunne, Loretta, additional, Dye, Simon, additional, Furlanetto, Cristina, additional, Holwerda, Benne, additional, Ivison, R J, additional, Kelvin, L S, additional, Lara-Lopez, Maritza, additional, Leeuw, Lerothodi, additional, Loveday, Jon, additional, Maddox, Steve, additional, Michałowski, Michał J, additional, Phillipps, Steven, additional, Robotham, Aaron, additional, Smith, Dan, additional, Smith, Matthew, additional, Valiante, Elisabetta, additional, van der Werf, Paul, additional, and Wright, Angus, additional

Published
2018
Full Text
View/download PDF

40. Galaxy and Mass Assembly (GAMA): variation in galaxy structure across the green valley

Author

Kelvin, Lee S, primary, Bremer, Malcolm N, additional, Phillipps, Steven, additional, James, Philip A, additional, Davies, Luke J M, additional, De Propris, Roberto, additional, Moffett, Amanda J, additional, Percival, Susan M, additional, Baldry, Ivan K, additional, Collins, Chris A, additional, Alpaslan, Mehmet, additional, Bland-Hawthorn, Joss, additional, Brough, Sarah, additional, Cluver, Michelle, additional, Driver, Simon P, additional, Hashemizadeh, Abdolhosein, additional, Holwerda, Benne W, additional, Laine, Jarkko, additional, Lara-Lopez, Maritza A, additional, Liske, Jochen, additional, Maciejewski, Witold, additional, Napolitano, Nicola R, additional, Penny, Samantha J, additional, Popescu, Cristina C, additional, Sansom, Anne E, additional, Sutherland, Will, additional, Taylor, Edward N, additional, van Kampen, Eelco, additional, and Wang, Lingyu, additional

Published
2018
Full Text
View/download PDF

41. The SAMI Galaxy Survey: spatially resolving the main sequence of star formation

Author

Medling, Anne M, primary, Cortese, Luca, additional, Croom, Scott M, additional, Green, Andrew W, additional, Groves, Brent, additional, Hampton, Elise, additional, Ho, I-Ting, additional, Davies, Luke J M, additional, Kewley, Lisa J, additional, Moffett, Amanda J, additional, Schaefer, Adam L, additional, Taylor, Edward, additional, Zafar, Tayyaba, additional, Bekki, Kenji, additional, Bland-Hawthorn, Joss, additional, Bloom, Jessica V, additional, Brough, Sarah, additional, Bryant, Julia J, additional, Catinella, Barbara, additional, Cecil, Gerald, additional, Colless, Matthew, additional, Couch, Warrick J, additional, Drinkwater, Michael J, additional, Driver, Simon P, additional, Federrath, Christoph, additional, Foster, Caroline, additional, Goldstein, Gregory, additional, Goodwin, Michael, additional, Hopkins, Andrew, additional, Lawrence, J S, additional, Leslie, Sarah K, additional, Lewis, Geraint F, additional, Lorente, Nuria P F, additional, Owers, Matt S, additional, McDermid, Richard, additional, Richards, Samuel N, additional, Sharp, Robert, additional, Scott, Nicholas, additional, Sweet, Sarah M, additional, Taranu, Dan S, additional, Tescari, Edoardo, additional, Tonini, Chiara, additional, van de Sande, Jesse, additional, Walcher, C Jakob, additional, and Wright, Angus, additional

Published
2018
Full Text
View/download PDF

44. MUSE spectroscopy and deep observations of a unique compact JWST target, lensing cluster CLIO

Author

Griffiths, Alex, primary, Conselice, Christopher J, additional, Alpaslan, Mehmet, additional, Frye, Brenda L, additional, Diego, Jose M, additional, Zitrin, Adi, additional, Yan, Haojing, additional, Ma, Zhiyuan, additional, Barone-Nugent, Robert, additional, Bhatawdekar, Rachana, additional, Driver, Simon P, additional, Robotham, Aaron S G, additional, Windhorst, Rogier A, additional, and Wyithe, J Stuart B, additional

Published
2018
Full Text
View/download PDF

45. The SAMI Galaxy Survey: Data Release One with emission-line physics value-added products

Author

Green, Andrew W, primary, Croom, Scott M, additional, Scott, Nicholas, additional, Cortese, Luca, additional, Medling, Anne M, additional, D'Eugenio, Francesco, additional, Bryant, Julia J, additional, Bland-Hawthorn, Joss, additional, Allen, J T, additional, Sharp, Rob, additional, Ho, I-Ting, additional, Groves, Brent, additional, Drinkwater, Michael J, additional, Mannering, Elizabeth, additional, Harischandra, Lloyd, additional, van de Sande, Jesse, additional, Thomas, Adam D, additional, O'Toole, Simon, additional, McDermid, Richard M, additional, Vuong, Minh, additional, Sealey, Katrina, additional, Bauer, Amanda E, additional, Brough, S, additional, Catinella, Barbara, additional, Cecil, Gerald, additional, Colless, Matthew, additional, Couch, Warrick J, additional, Driver, Simon P, additional, Federrath, Christoph, additional, Foster, Caroline, additional, Goodwin, Michael, additional, Hampton, Elise J, additional, Hopkins, A M, additional, Jones, D Heath, additional, Konstantopoulos, Iraklis S, additional, Lawrence, J S, additional, Leon-Saval, Sergio G, additional, Liske, Jochen, additional, López-Sánchez, Ángel R, additional, Lorente, Nuria P F, additional, Mould, Jeremy, additional, Obreschkow, Danail, additional, Owers, Matt S, additional, Richards, Samuel N, additional, Robotham, Aaron S G, additional, Schaefer, Adam L, additional, Sweet, Sarah M, additional, Taranu, Dan S, additional, Tescari, Edoardo, additional, Tonini, Chiara, additional, and Zafar, T, additional

Published
2017
Full Text
View/download PDF

46. GAMA/G10-COSMOS/3D-HST: the 0 < z < 5 cosmic star formation history, stellar-mass, and dust-mass densities

Author

Driver, Simon P, primary, Andrews, Stephen K, additional, da Cunha, Elisabete, additional, Davies, Luke J, additional, Lagos, Claudia, additional, Robotham, Aaron S G, additional, Vinsen, Kevin, additional, Wright, Angus H, additional, Alpaslan, Mehmet, additional, Bland-Hawthorn, Joss, additional, Bourne, Nathan, additional, Brough, Sarah, additional, Bremer, Malcolm N, additional, Cluver, Michelle, additional, Colless, Matthew, additional, Conselice, Christopher J, additional, Dunne, Loretta, additional, Eales, Steve A, additional, Gomez, Haley, additional, Holwerda, Benne, additional, Hopkins, Andrew M, additional, Kafle, Prajwal R, additional, Kelvin, Lee S, additional, Loveday, Jon, additional, Liske, Jochen, additional, Maddox, Steve J, additional, Phillipps, Steven, additional, Pimbblet, Kevin, additional, Rowlands, Kate, additional, Sansom, Anne E, additional, Taylor, Edward, additional, Wang, Lingyu, additional, and Wilkins, Stephen M, additional

Published
2017
Full Text
View/download PDF

47. Galaxy And Mass Assembly: automatic morphological classification of galaxies using statistical learning

Author

Sreejith, Sreevarsha, primary, Pereverzyev Jr, Sergiy, additional, Kelvin, Lee S, additional, Marleau, Francine R, additional, Haltmeier, Markus, additional, Ebner, Judith, additional, Bland-Hawthorn, Joss, additional, Driver, Simon P, additional, Graham, Alister W, additional, Holwerda, Benne W, additional, Hopkins, Andrew M, additional, Liske, Jochen, additional, Loveday, Jon, additional, Moffett, Amanda J, additional, Pimbblet, Kevin A, additional, Taylor, Edward N, additional, Wang, Lingyu, additional, and Wright, Angus H, additional

Published
2017
Full Text
View/download PDF

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

Author

Eales, Stephen, primary, Smith, Dan, additional, Bourne, Nathan, additional, Loveday, Jon, additional, Rowlands, Kate, additional, van der Werf, Paul, additional, Driver, Simon, additional, Dunne, Loretta, additional, Dye, Simon, additional, Furlanetto, Cristina, additional, Ivison, R. J., additional, Maddox, Steve, additional, Robotham, Aaron, additional, Smith, Matthew W. L., additional, Taylor, Edward N., additional, Valiante, Elisabetta, additional, Wright, Angus, additional, Cigan, Philip, additional, De Zotti, Gianfranco, additional, Jarvis, Matt J., additional, Marchetti, Lucia, additional, Michałowski, Michał J., additional, Phillipps, Steven, additional, Viaene, Sebastien, additional, and Vlahakis, Catherine, additional

Published
2017
Full Text
View/download PDF

49. Galaxy and Mass Assembly (GAMA): halo formation times and halo assembly bias on the cosmic web

Author

Tojeiro, Rita, primary, Eardley, Elizabeth, additional, Peacock, John A., additional, Norberg, Peder, additional, Alpaslan, Mehmet, additional, Driver, Simon P., additional, Henriques, Bruno, additional, Hopkins, Andrew M., additional, Kafle, Prajwal R., additional, Robotham, Aaron S. G., additional, Thomas, Peter, additional, Tonini, Chiara, additional, and Wild, Vivienne, additional

Published
2017
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results