PHYSICAL PROPERTIES OF COMPACT STAR-FORMING GALAXIES AT<i>z</i>∼ 2–3

Fang, Guanwen; Ma, Z.Y.; Kong, Xu; Fan, Lulu

doi:10.1088/0004-637x/807/2/139

Cited by 20 publications

(52 citation statements)

References 69 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It is clear that the fraction of these cSFGs decrease with redshift, which is a strong evidence that some of these cSFGs are translating into cQGs. It is reported in Fang et al (2015) that cSFGs also have slightly lower SFRs than eSFGs at 2 < z < 3 . It supports that the overall star-forming status for cSFGs are turning down with the decrease of redshift, which implies that the cSFGs at the lower redshift are more likely to be quenched.…”

Section: The Sfr−m * Relationmentioning

confidence: 84%

Structures, Stellar Population Properties, AGN Fractions, and Environments of Massive Compact Galaxies at 1 < z < 2 in 3D-HST/CANDELS

Fang

Yuan

et al. 2020

PASP

Self Cite

View full text Add to dashboard Cite

We present a study on structures and physical properties of massive (M * > 10 10 M ⊙ ) compact galaxies at 1.0 < z < 2.0 in five 3D-HST/CANDELS fields. Compared with the extended star-forming galaxies (eSFGs), compact star-forming galaxies (cSFGs) are found to have the lower level of star formation, and mainly distribute in the quiescent region of the UVJ diagram. The distributions of dust attenuation and Sérsic index support that the progenitors of cQGs are cSFGs, and cSFGs are at a transitional phase between eSFGs and cQGs. The prevalence of X-ray selected AGNs (∼ 28%) is confirmed in the cSFGs at 1 < z < 2 which indicates that the violent gas-rich processes such as merger and disk instability could drive the structure to be more compact, and trigger both star formation and black hole growth in the central regions. Our results support the "two-step" scenario that the cSFGs at 1 < z < 2 are the intermediate population after compaction but before a quick quenching. Our analysis of parametric and nonparametric morphologies shows that cQGs (eQGs) are more concentrated and have less substructures than cSFGs (eSFGs), and quenching and compactness should be associated with each other. The cSFGs at 1.5 < z < 2 (1 < z < 1.5) prefer to be in higher (lower) density environment, similar as cQGs (eSFGs). It suggests that merger or strong interaction might be the main driving mechanism of compaction at higher redshifts, whereas the disk instability of individual galaxies might play a more important role on the formation of cSFGs at lower redshifts.

show abstract

Section: The Sfr−m * Relationmentioning

confidence: 84%

Structures, Stellar Population Properties, AGN Fractions, and Environments of Massive Compact Galaxies at 1 < z < 2 in 3D-HST/CANDELS

Fang

Yuan

et al. 2020

PASP

Self Cite

View full text Add to dashboard Cite

show abstract

“…These include the compact SFGs (cSFGs) at z 2 to z ∼ 4 (e.g. Barro et al 2013;Patel et al 2013;Stefanon et al 2013;Barro et al 2014;Fang et al 2015;van Dokkum et al 2015;Spilker et al 2016), and the passive, V JL selected galaxies at z = 2.5 − 4, which tend to be disk-dominated (Fan et al 2013). Toft et al (2014) speculated that the Barro et al (2013) cSFGs at z 3 might represent a transition phase between some of the z 3 SMGs and z ∼ 2 cQGs.…”

Section: Comparison Of the Physical Properties Between Different Galamentioning

confidence: 99%

An ALMA survey of submillimetre galaxies in the COSMOS field: Physical properties derived from energy balance spectral energy distribution modelling

Miettinen

Delvecchio

Smolčić

et al. 2017

A&A

View full text Add to dashboard Cite

Context. Submillimetre galaxies (SMGs) represent an important source population in the origin and cosmic evolution of the most massive galaxies. Hence, it is imperative to place firm constraints on the fundamental physical properties of large samples of SMGs. Aims. We determine the physical properties of a sample of SMGs in the COSMOS field that were pre-selected at the observed-frame wavelength of λ obs = 1.1 mm, and followed up at λ obs = 1.3 mm with the Atacama Large Millimetre/submillimetre Array (ALMA). Methods. We used the MAGPHYS model package to fit the panchromatic (ultraviolet to radio) spectral energy distributions (SEDs) of 124 of the target SMGs, which lie at a median redshift of z = 2.30 (19.4% are spectroscopically confirmed). The SED analysis was complemented by estimating the gas masses of the SMGs by using the λ obs = 1.3 mm dust emission as a tracer of the molecular gas component.Results. The sample median and 16th-84th percentile ranges of the stellar masses, obscured star formation rates, dust temperatures, and dust and gas masses were derived to be log(−0.31 , and log(M gas /M ⊙ ) = 11.34 +0.20 −0.23 , respectively. The M dust /M ⋆ ratio was found to decrease as a function of redshift, while the M gas /M dust ratio shows the opposite, positive correlation with redshift. The derived median gas-to-dust ratio of 120 +73 −30 agrees well with the canonical expectation. The gas fraction (M gas /(M gas + M ⋆ )) was found to range from 0.10 to 0.98 with a median of 0.62 +0.27 −0.23 . We found that 57.3% of our SMGs populate the main sequence (MS) of star-forming galaxies, while 41.9% of the sources lie above the MS by a factor of greater than three (one source lies below the MS). These super-MS objects, or starbursts, are preferentially found at z 3, which likely reflects the sensitivity limit of our source selection. We estimated that the median gas consumption timescale for our SMGs is ∼ 535 Myr, and the super-MS sources appear to consume their gas reservoir faster than their MS counterparts. We found no obvious stellar mass-size correlations for our SMGs, where the sizes were measured in the observed-frame 3 GHz radio emission and rest-frame UV. However, the largest 3 GHz radio sizes are found among the MS sources. Those SMGs that appear irregular in the rest-frame UV are predominantly starbursts, while the MS SMGs are mostly disk-like. Conclusions. The physical parameter distributions of our SMGs and those of the equally bright, 870 µm selected SMGs in the ECDFS field (the so-called ALESS SMGs) are unlikely to be drawn from common parent distributions. This might reflect the difference in the pre-selection wavelength. Albeit being partly a selection bias, the abrupt jump in specific SFR and the offset from the MS of our SMGs at z 3 might also reflect a more efficient accretion from the cosmic gas streams, higher incidence of gas-rich major mergers, or higher star formation efficiency at z 3. We found a rather flat average trend between the SFR and dust mass, but a positive SFR − M gas correlatio...

show abstract

“…Of course, morphological disturbance above the main sequence is not universal; see Barro et al (2016)). 3) Compact star-forming galaxies (cSFGs, as defined in Barro et al (2013)) on or just below the main sequence at z∼ 2-3 suggest that bulge growth precedes quenching (Barro et al 2014;Williams et al 2014;Fang et al 2015). Fang et al (2015) even found that at z∼ 2-3, cSFGs dominate the high mass end of the main sequence.…”

mentioning

confidence: 99%

“…3) Compact star-forming galaxies (cSFGs, as defined in Barro et al (2013)) on or just below the main sequence at z∼ 2-3 suggest that bulge growth precedes quenching (Barro et al 2014;Williams et al 2014;Fang et al 2015). Fang et al (2015) even found that at z∼ 2-3, cSFGs dominate the high mass end of the main sequence. 4) Quiescence is almost always associated with a bulge component or high central stellar mass density or velocity dispersion (Franx et al 2008;Bell et al 2012;Wake et al 2012;Fang et al 2013;Bluck et al 2014;Lang et al 2014;Woo et al 2015;Teimoorinia et al 2016).…”

mentioning

confidence: 99%

The relationship between star formation activity and galaxy structural properties in CANDELS and a semi-analytic model

Brennan

Pandya

Somerville

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We study the correlation of galaxy structural properties with their location relative to the SFR-M * correlation, also known as the star formation "main sequence" (SFMS), in the CANDELS and GAMA surveys and in a semi-analytic model (SAM) of galaxy formation. We first study the distribution of median Sérsic index, effective radius, star formation rate (SFR) density and stellar mass density in the SFR-M * plane. We then define a redshift dependent main sequence and examine the medians of these quantities as a function of distance from this main sequence, both above (higher SFRs) and below (lower SFRs). Finally, we examine the distributions of distance from the main sequence in bins of these quantities. We find strong correlations between all of these galaxy structural properties and the distance from the SFMS, such that as we move from galaxies above the SFMS to those below it, we see a nearly monotonic trend towards higher median Sérsic index, smaller radius, lower SFR density, and higher stellar density. In the semi-analytic model, bulge growth is driven by mergers and disk instabilities, and is accompanied by the growth of a supermassive black hole which can regulate or quench star formation via Active Galactic Nucleus (AGN) feedback. We find that our model qualitatively reproduces the trends described above, supporting a picture in which black holes and bulges co-evolve, and AGN feedback plays a critical role in moving galaxies off of the SFMS.

show abstract

PHYSICAL PROPERTIES OF COMPACT STAR-FORMING GALAXIES ATz∼ 2–3

Cited by 20 publications

References 69 publications

Structures, Stellar Population Properties, AGN Fractions, and Environments of Massive Compact Galaxies at 1 < z < 2 in 3D-HST/CANDELS

Structures, Stellar Population Properties, AGN Fractions, and Environments of Massive Compact Galaxies at 1 < z < 2 in 3D-HST/CANDELS

An ALMA survey of submillimetre galaxies in the COSMOS field: Physical properties derived from energy balance spectral energy distribution modelling

The relationship between star formation activity and galaxy structural properties in CANDELS and a semi-analytic model

Contact Info

Product

Resources

About