Environmental dependence of local luminous infrared galaxies

Hwang, Ho Seong; Elbaz, D.; Lee, Jong Chul; Jeong, Wooju; Park, Changbom; Lee, Myung Gyoon; Lee, Hyung Mok

doi:10.1051/0004-6361/201014807

Cited by 75 publications

(86 citation statements)

References 88 publications

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“…Although SDSS surveys a huge field, there is some residual incompleteness in dense regions due to fiber collisions (Strauss et al 2002;Park & Hwang 2009;Shen et al 2016). We thus compile missing redshifts from the literature, mainly from NED (for more details, see Hwang et al 2010). In total, we compile 22410 redshifts within < ¢ R 300…”

Section: Comamentioning

confidence: 99%

The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma

Sohn¹,

Geller²,

Zahid³

et al. 2017

ApJS

107

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Based on an extensive redshift survey for galaxy clusters Abell 2029 and Coma, we measure the luminosity functions (LFs) and stellar mass functions (SMFs) for the entire cluster member galaxies. Most importantly, we measure the velocity dispersion functions (VDFs) for quiescent members. The MMT/Hectospec redshift survey for galaxies in A2029 identifies 982 spectroscopic members; for 838 members, we derive the central velocity dispersion from the spectroscopy. Coma is the only other cluster surveyed as densely. The LFs, SMFs, and VDFs for A2029 and Coma are essentially identical. The SMFs of the clusters are consistent with simulations. The A2029 and Coma VDFs for quiescent galaxies have a significantly steeper slope than those of field galaxies for velocity dispersion  -100 km s 1 . The cluster VDFs also exceed the field at velocity dispersion  -250 km s 1 . The differences between cluster and field VDFs are potentially important tests of simulations and of the formation of structure in the universe.

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Section: Comamentioning

confidence: 99%

The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma

Sohn¹,

Geller²,

Zahid³

et al. 2017

ApJS

107

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“…The SFRs of galaxies are known to depend strongly on the local density in the sense that spatially averaged SFRs of galaxies or star-forming galaxy fractions decrease as the background density increases in the local universe (e.g., Lewis et al 2002;Gómez et al 2003;Park et al 2007;Lee et al 2010;Hwang et al 2010a). In the high-z universe, some studies found similar results (e.g., Patel et al 2009;Feruglio et al 2010), but there are also hints for an opposite trend (i.e.…”

Section: Fig 6 Same Asmentioning

confidence: 99%

“…Many studies have extensively investigated this enhancement of SFA in paired galaxies Article published by EDP Sciences A60, page 1 of 10 (e.g., Condon et al 1982;Keel et al 1985;Kennicutt et al 1987;Barton et al 2000;Lambas et al 2003;Nikolic et al 2004;Alonso et al 2004;De Propris et al 2005;Geller et al 2006;Woods & Geller 2007;Li et al 2008;Ellison et al 2008;Knapen & James 2009;Perez et al 2009;Park & Choi 2009;Hwang et al 2010a;Xu et al 2010;Darg et al 2010;Patton et al 2011). In summary, the SFA of galaxies seems to strongly depend on the morphology and the mutual separation of galaxies in pairs.…”

Section: Introductionmentioning

confidence: 99%

GOODS-Herschel: the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies

Hwang¹,

Elbaz²,

Dickinson³

et al. 2011

A&A

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Aims. We study the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies and its evolution at 0 < z < 1.2. Methods. Using the high-z galaxies in the fields of Great Observatories Origins Deep Survey (GOODS) observed by the Herschel Space Observatory in the framework of the GOODS-Herschel key program and the local IRAS or AKARI-selected galaxies in the field of Sloan Digital Sky Survey Data Release 7, we investigate the dependence of galaxy properties on the morphology of and the distance to the nearest neighbor galaxy. Results. We find that the star-formation rates (SFRs) and the specific SFRs (SSFRs) of galaxies on average depend on the morphology of and the distance to the nearest neighbor galaxy in this redshift range. When a late-type galaxy has a close neighbor galaxy, the SFR and the SSFR increase as it approaches a late-type neighbor, which is supported by Kolmogorov-Smirnov (K-S) and Monte Carlo (MC) tests with a significance level of >99%. However, the SFR and the SSFR decrease or do not change much as the galaxy approaches an early-type neighbor. The bifurcations of SFRs and SSFRs depending on the neighbor's morphology seem to occur at R n ≈ 0.5r vir,nei (virial radius of the neighbor), which is supported by K-S and MC tests with a significance level of >98%. For all redshift bins, the SSFRs of late-type galaxies interacting with late-type neighbors are increased by factors of about 1.8 ± 0.7 and 4.0 ± 1.2 compared to those of non-interacting galaxies when the pair separation is smaller than 0.5r vir,nei and 0.1r vir,nei , respectively. The dust temperature of both local and high-z late-type galaxies that strongly interact with late-type neighbors (i.e. R n ≤ 0.1r vir,nei ) appears to be higher than that of non-interacting galaxies with a significance level of 96−99%. However, the dust temperature of local late-type galaxies that strongly interact with early-type neighbors seems to be lower than or similar to that of non-interacting galaxies. Conclusions. Our results suggest that galaxy-galaxy interactions and mergers have been strongly affecting the SFR and the dust properties of star-forming galaxies over at least 8 billion years.

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“…Though galaxies undergoing a starburst event are commonly associated with a late-type morphology (i.e., spiral, irregular, or chaotic), a non-negligible fraction of starbursts are, surprisingly, associated with early-types (Mobasher et al 2004;Poggianti et al 2009;Abramson et al 2013). Additionally, starbursts are observed in hosts that span a wide range of stellar masses (e.g., Lehnert & Heckman 1996;Elbaz et al 2011, Hilton et al 2012Ibar et al 2013), color properties (e.g., Kartaltepe et al 2010b;Kocevski et al 2011a), and environments (e.g., Marcillac et al 2008;Gallazzi et al 2009;Hwang et al 2010a;Lemaux et al 2012;Dressler et al 2013). And though some starbursting populations show morphologies indicative of a recent merging or tidal interactions, others appear primarily as undisturbed, grand-design spirals, with little evidence of recent interactions with their surroundings (see, e.g., Ravindranath et al 2006;Kocevski et al 2011a;Tadhunter et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

Lemaux

Floc’h

Fèvre

et al. 2014

A&A

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We investigate of the properties of ∼2000 Herschel/SPIRE far-infrared-selected galaxies from 0 < z < 4 in the CFHTLS-D1 field. Using a combination of extensive spectroscopy from the VVDS and ORELSE surveys, deep multiwavelength imaging from CFHT, VLA, Spitzer, XMM-Newton, and Herschel, and well-calibrated spectral energy distribution fitting, Herschel-bright galaxies are compared to optically-selected galaxies at a variety of redshifts. Herschel-selected galaxies are observed to span a range of stellar masses, colors, and absolute magnitudes equivalent to galaxies undetected in SPIRE. Though many Herschel galaxies appear to be in transition, such galaxies are largely consistent with normal star-forming galaxies when rest-frame colors are utilized. The nature of the star-forming "main sequence" is studied and we warn against adopting this framework unless the main sequence is determined precisely. Herschel galaxies at different total infrared luminosities (L TIR ) are compared. Bluer optical colors, larger nebular extinctions, and larger contributions from younger stellar populations are observed for galaxies with larger L TIR , suggesting that low-L TIR galaxies are undergoing rejuvenated starbursts while galaxies with higher L TIR are forming a larger percentage of their stellar mass. A variety of methods are used to select powerful active galactic nuclei (AGN). Galaxies hosting all types of AGN are observed to be undergoing starbursts more commonly and vigorously than a matched sample of galaxies without powerful AGN and, additionally, the fraction of galaxies with an AGN increases with increasing star formation rate at all redshifts. At all redshifts (0 < z < 4) the most prodigious star-forming galaxies are found to contain the highest fraction of powerful AGN. For redshift bins that allow a comparison (z > 0.5), the highest L TIR galaxies in a given redshift bin are unobserved by SPIRE at subsequently lower redshifts, a trend linked to downsizing. In conjunction with other results, this evidence is used to argue for prevalent AGN-driven quenching in starburst galaxies across cosmic time.

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Environmental dependence of local luminous infrared galaxies

Cited by 75 publications

References 88 publications

The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma

The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma

GOODS-Herschel: the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

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