Assembly bias evidence in close galaxy pairs
Abstract
ABSTRACT The growth channel of massive galaxies involving mergers can be studied via close pairs as putative merger progenitors, where the stellar populations of the satellite galaxies will be eventually incorporated into the massive primaries. We extend our recent analysis of the GAMA-based sample of close pairs presented in Ferreras et al. to the general spectroscopic data set of SDSS galaxies (DR14), for which the high S/N of the data enables a detailed analysis of the differences between satellite galaxies with respect to the mass of the primary galaxy. A sample of approximately 2000 satellites of massive galaxies is carefully selected within a relatively narrow redshift range (0.07<z<0.14). Two main parameters are considered as major drivers of the star formation history of these galaxies, namely: the stellar velocity dispersion of the satellite (σ), as a proxy of ‘local’ drivers, and the ratio between the stellar mass of the satellite and the primary, μ = MSAT/MPRI, meant to serve as an indicator of environment. Consistently with the independent, GAMA-based work, we find that satellites around the most massive primaries appear older, at fixed velocity dispersion, than satellites of lower mass primaries. This trend is more marked in lower mass satellites (σ ∼ 100 km s−1),more »
- Authors:
-
[3];
[4];
[5];
[5];
[6]
- Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UK, Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK, Instituto de Astrofísica de Canarias, Calle Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain, Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain
- Australian Astronomical Optics, Macquarie University, 105 Delhi Rd, North Ryde, NSW 2113, Australia
- ICRAR, M468, University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia
- Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK
- Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney, Sydney, NSW 2006, Australia, ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)
- School of Physics, University of New South Wales, NSW 2052, Australia
- Publication Date:
- Sponsoring Org.:
- USDOE
- OSTI Identifier:
- 1515609
- Resource Type:
- Published Article
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 487 Journal Issue: 1; Journal ID: ISSN 0035-8711
- Publisher:
- Oxford University Press
- Country of Publication:
- United Kingdom
- Language:
- English
Citation Formats
Ferreras, I., Hopkins, A. M., Lagos, C., Sansom, A. E., Scott, N., Croom, S., and Brough, S. Assembly bias evidence in close galaxy pairs. United Kingdom: N. p., 2019.
Web. doi:10.1093/mnras/stz1286.
Ferreras, I., Hopkins, A. M., Lagos, C., Sansom, A. E., Scott, N., Croom, S., & Brough, S. Assembly bias evidence in close galaxy pairs. United Kingdom. https://doi.org/10.1093/mnras/stz1286
Ferreras, I., Hopkins, A. M., Lagos, C., Sansom, A. E., Scott, N., Croom, S., and Brough, S. Sat .
"Assembly bias evidence in close galaxy pairs". United Kingdom. https://doi.org/10.1093/mnras/stz1286.
@article{osti_1515609,
title = {Assembly bias evidence in close galaxy pairs},
author = {Ferreras, I. and Hopkins, A. M. and Lagos, C. and Sansom, A. E. and Scott, N. and Croom, S. and Brough, S.},
abstractNote = {ABSTRACT The growth channel of massive galaxies involving mergers can be studied via close pairs as putative merger progenitors, where the stellar populations of the satellite galaxies will be eventually incorporated into the massive primaries. We extend our recent analysis of the GAMA-based sample of close pairs presented in Ferreras et al. to the general spectroscopic data set of SDSS galaxies (DR14), for which the high S/N of the data enables a detailed analysis of the differences between satellite galaxies with respect to the mass of the primary galaxy. A sample of approximately 2000 satellites of massive galaxies is carefully selected within a relatively narrow redshift range (0.07<z<0.14). Two main parameters are considered as major drivers of the star formation history of these galaxies, namely: the stellar velocity dispersion of the satellite (σ), as a proxy of ‘local’ drivers, and the ratio between the stellar mass of the satellite and the primary, μ = MSAT/MPRI, meant to serve as an indicator of environment. Consistently with the independent, GAMA-based work, we find that satellites around the most massive primaries appear older, at fixed velocity dispersion, than satellites of lower mass primaries. This trend is more marked in lower mass satellites (σ ∼ 100 km s−1), with SSP-equivalent age differences up to ∼0.5 Gyr, and can be interpreted as a one-halo assembly bias, so that satellites corresponding to smaller values of μ represent older structures, akin to fossil groups.},
doi = {10.1093/mnras/stz1286},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 1,
volume = 487,
place = {United Kingdom},
year = {Sat May 11 00:00:00 EDT 2019},
month = {Sat May 11 00:00:00 EDT 2019}
}
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