Star formation rates in isolated galaxies selected from the Two-Micron All-Sky Survey

Мelnyk, О. V.; Караченцева, В. Е.; Караченцев, И. Д.

doi:10.1093/mnras/stv950

Cited by 14 publications

(15 citation statements)

References 96 publications

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“…For massive galaxies, the fraction of optical AGN in the SIG and SIP samples is slightly higher than in control samples. In particular, the fraction of optical AGN for massive isolated galaxies is higher than in any other sample, which is discrepant with Melnyk et al (2015), who found the fraction of AGN in pairs is only a little higher than in isolated galaxies.…”

Section: Optical Agncontrasting

confidence: 95%

The effect of local and large-scale environments on nuclear activity and star formation

Argudo-Fernández

Shen

Sabater

et al. 2016

A&A

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Context. Active galactic nuclei (AGN) are one of the main drivers for the transition from star-forming disk to passive spheroidal galaxies, however, the role of large-scale environment versus one-on-one interactions in triggering different types of AGN is still uncertain. We present a statistical study of the prevalence of the nuclear activity in isolated galaxies and physically bound isolated pairs. Aims. For the purpose of this study we considered optically and radio selected nuclear activity types. We aim to assess the effect of one-on-one interaction on the fraction of AGN and the role of their large-scale environment. Methods. To study the effect of one-on-one interaction on the fraction of AGN in isolated galaxy pairs, we compare these AGN with a sample of isolated galaxies homogeneously selected under the same isolation criterion. We examine the effect of the largescale environment by comparing isolated systems with control samples of single galaxies and galaxy pairs. We use the tidal strength parameter to quantify the effects of local and large-scale environments. Results. In general we found no difference in the prevalence of optical AGN for the considered samples. For massive galaxies, the fraction of optical AGN in isolated galaxies is slightly higher than that in the control samples. Also, the fraction of passives in high mass isolated galaxies is smaller than in any other sample. Generally, there is no dependence on optical nuclear activity with local environment. On the other hand, we found evidence that radio AGN are strongly affected by the local environment. Conclusions. The optical AGN phenomenon is related to cold gas accretion, while radio AGN are related to hot gas accretion. In this context, there is more cold gas, fuelling the central optical AGN, in isolated systems. Our results are in agreement with a scenario where cold gas accretion by secular evolution is the main driver of optical AGN, while hot gas accretion and one-on-one interactions are the main drivers of radio AGN activity.

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Section: Optical Agncontrasting

confidence: 95%

The effect of local and large-scale environments on nuclear activity and star formation

Argudo-Fernández

Shen

Sabater

et al. 2016

A&A

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“…The dependence of the MS on the large scale environment is still under discussion, however a clear correlation seems to exist between SFR and paired galaxies. Melnyk et al (2015) found that paired massive (log(M * /M ) > 11.5) galaxies have higher SFR than isolated galaxies, and this same result was found for lower mass galaxies with the galaxy pairs in the Sloan Digital Sky Survey (e.g. Ellison et al 2010;Scudder et al 2012b) and for major-merger pairs in Herschel (Cao et al 2015).…”

Section: Introductionmentioning

confidence: 74%

HELP: star formation as a function of galaxy environment withHerschel

Duivenvoorden¹,

Oliver²,

Buat³

et al. 2016

Mon. Not. R. Astron. Soc.

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The Herschel Extragalactic Legacy Project (HELP) brings together a vast range of data from many astronomical observatories. Its main focus is on the Herschel data, which maps dust obscured star formation over 1300 deg 2 . With this unprecedented combination of data sets, it is possible to investigate how the star formation vs stellar mass relation (main-sequence) of star-forming galaxies depends on environment. In this pilot study we explore this question between 0.1 < z < 3.2 using data in the COSMOS field. We estimate the local environment from a smoothed galaxy density field using the full photometric redshift probability distribution. We estimate star formation rates by stacking the SPIRE data from the Herschel Multi-tiered Extragalactic Survey (HerMES). Our analysis rules out the hypothesis that the main-sequence for starforming systems is independent of environment at 1.5 < z < 2, while a simple model in which the mean specific star formation rate declines with increasing environmental density gives a better description. However, we cannot exclude a simple hypothesis in which the main-sequence for star-forming systems is independent of environment at z < 1.5 and z > 2. We also estimate the evolution of the star formation rate density in the COSMOS field and our results are consistent with previous measurements at z < 1.5 and z > 2 but we find a 1.4 +0.3 −0.2 times higher peak value of the star formation rate density at z ∼ 1.9.

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“…4) We can also estimate the absolute K-magnitude from the calibration relation (3) considering the additional relation (4) for the galaxies without direct V m measurements. we marked earlier [19][20][21] as a certain quasi-"Eddington" limit for the star formation intensity at the present epoch. Above this limit there are only a few galaxies, the K-luminosity (stellar mass) of which is underestimated from the As it can be seen, the behavior of dependences for flat and ultra-flat galaxies is approximately the same.…”

Section: Galaxy Stellar Mass Estimationmentioning

confidence: 81%

“…Considering the sample of isolated galaxies from the 2MIG catalog [23], Melnyk et al [21] obtained the mean parameters P = −0.62 ± 0.02 and F = −0.14 ± 0.02. The P value for 2MIG galaxies coincides within the errors with the mean −0.65 ± 0.03 for flat galaxies.…”

Section: Twomentioning

confidence: 99%

“…For the galaxies of the nearby universe within D ∼ 50 Mpc the upper limit of specific star formation rate was found, log sSF R = −9.4 yr −1 [19][20][21]. This condition is met for the Local Volume galaxies (D < 10 Mpc), located in the environments of different density [19], as well as for the LOG [22] and 2MIG [23] catalogs of isolated galaxies, having the depth of z ∼ 0.01.…”

Section: Introductionmentioning

confidence: 99%

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Ultra-flat galaxies selected from RFGC catalog. III. Star formation rate

2017

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We examine the star formation properties of galaxies with very thin disks selected from the Revised Flat Galaxy Catalog (RFGC). The sample contains 333 ultra-flat galaxies (UFG) at high Galactic latitudes, |b| > 10 • , with a blue major angular diameter of a ≥ 1. ′ 2, blue and red apparent axial ratios of (a/b) b > 10, (a/b) r > 8.5 and radial velocities within 10 000 km s −1. As a control sample for them we use a population of 722 more thick RFGC galaxies with (a/b) b > 7, situated in the same volume. The UFG distribution over the sky indicates them as a population of quite isolated galaxies. We found that the specific star formation rate, sSF R FUV , determined via the FUV GALEX flux, increases steadily from the early type to late type disks for both the UFG and RFGC-UFG samples, showing no significant mutual difference within each morphological type T. The population of UFG disks has the average H I-mass-to-stellar-mass ratio by (0.25 ± 0.03) dex higher than that of RFGC-UFG galaxies. Being compared with arbitrary orientated disks of the same type, the ultra-flat edge-on galaxies reveal that their total H I mass is hidden by self-absorption on the average by approximately 0.20 dex. We demonstrate that using the robust stellar mass estimate via B − K-color and galaxy type T for the thin disks, together with a nowaday accounting for internal extinction, yields their sSF R quantities definitely lying below the limit of −9.4 dex (yr −1). The collected observational data on UFG disks imply that their average star formation rate in the past has been approximately three times the current SF R. The UFG galaxies have also sufficient amount of gas to support their observed SF R over the following nearly 9 Gyrs.

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Star formation rates in isolated galaxies selected from the Two-Micron All-Sky Survey

Cited by 14 publications

References 96 publications

The effect of local and large-scale environments on nuclear activity and star formation

The effect of local and large-scale environments on nuclear activity and star formation

HELP: star formation as a function of galaxy environment withHerschel

Ultra-flat galaxies selected from RFGC catalog. III. Star formation rate

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