- ID:
- ivo://CDS.VizieR/J/ApJ/675/234
- Title:
- Stellar mass functions for galaxies 0<z<4
- Short Name:
- J/ApJ/675/234
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using a sample of ~28000 sources selected at 3.6-4.5um with Spitzer observations of the Hubble Deep Field North, the Chandra Deep Field South, and the Lockman Hole (surveyed area ~664arcmin^2^), we study the evolution of the stellar mass content of the universe at 0<z<4. We calculate stellar masses and photometric redshifts, based on ~2000 templates built with stellar population and dust emission models fitting the ultraviolet to mid-infrared spectral energy distributions of galaxies with spectroscopic redshifts. We estimate stellar mass functions for different redshift intervals.
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- ID:
- ivo://CDS.VizieR/J/ApJ/777/18
- Title:
- Stellar mass functions of galaxies to z=4
- Short Name:
- J/ApJ/777/18
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present measurements of the stellar mass functions (SMFs) of star-forming and quiescent galaxies to z=4 using a sample of 95675 K_s_-selected galaxies in the COSMOS/UltraVISTA field (Muzzin et al. 2013ApJS..206....8M). The SMFs of the combined population are in good agreement with previous measurements and show that the stellar mass density of the universe was only 50%, 10%, and 1% of its current value at z~0.75, 2.0, and 3.5, respectively. The quiescent population drives most of the overall growth, with the stellar mass density of these galaxies increasing as {rho}_star_{prop.to}(1+z)^-4.7+/-0.4^ since z=3.5, whereas the mass density of star-forming galaxies increases as {rho}_star_{prop.to}(1+z)^-2.3 +/-0.2^. At z>2.5, star-forming galaxies dominate the total SMF at all stellar masses, although a non-zero population of quiescent galaxies persists to z=4. Comparisons of the K_s_-selected star-forming galaxy SMFs with UV-selected SMFs at 2.5<z<4 show reasonable agreement and suggest that UV-selected samples are representative of the majority of the stellar mass density at z>3.5. We estimate the average mass growth of individual galaxies by selecting galaxies at fixed cumulative number density. The average galaxy with log(M_star_/M_{sun}_)=11.5 at z=0.3 has grown in mass by only 0.2dex (0.3dex) since z=2.0 (3.5), whereas those with log(M_star_/M_{sun}_)=10.5 have grown by >1.0dex since z=2. At z<2, the time derivatives of the mass growth are always larger for lower-mass galaxies, which demonstrates that the mass growth in galaxies since that redshift is mass-dependent and primarily bottom-up. Lastly, we examine potential sources of systematic uncertainties in the SMFs and find that those from photo-z templates, stellar population synthesis modeling, and the definition of quiescent galaxies dominate the total error budget in the SMFs.
- ID:
- ivo://CDS.VizieR/J/A+A/610/A5
- Title:
- Stellar structure models of edge-on galaxies
- Short Name:
- J/A+A/610/A5
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Recent studies have made the community aware of the importance of accounting for scattered light when examining low-surface-brightness galaxy features such as thick discs. In our past studies of the thick discs of edge-on galaxies in the Spitzer Survey of Stellar Structure in Galaxies - the S4G - we modelled the point spread function as a Gaussian. In this paper we re- examine our results using a revised point spread function model that accounts for extended wings out to more than 2.5arcmin. We study the 3.6micron images of 141 edge-on galaxies from the S4G and its early-type galaxy extension. Thus, we more than double the samples examined in our past studies. We decompose the surface-brightness profiles of the galaxies perpendicular to their mid-planes assuming that discs are made of two stellar discs in hydrostatic equilibrium. We decompose the axial surface- brightness profiles of galaxies to model the central mass concentration - described by a Sersic function - and the disc - described by a broken exponential disc seen edge-on. Our improved treatment fully confirms the ubiquitous occurrence of thick discs. The main difference between our current fits and those presented in our previous papers is that now the scattered light from the thin disc dominates the surface brightness at levels below ~26mag/arcsec^2^. We stress that those extended thin disc tails are not physical, but pure scattered light. This change, however, does not drastically affect any of our previously presented results: 1) Thick discs are nearly ubiquitous. They are not an artefact caused by scattered light as has been suggested elsewhere. 2) Thick discs have masses comparable to those of thin discs in low-mass galaxies - with circular velocities vc<120km/s - whereas they are typically less massive than the thin discs in high-mass galaxies. 3) Thick discs and central mass concentrations seem to have formed at the same epoch from a common material reservoir. 4) Approximately 50% of the up-bending breaks in face-on galaxies are caused by the superposition of a thin and a thick disc where the scale-length of the latter is the largest.
- ID:
- ivo://CDS.VizieR/J/ApJ/702/1567
- Title:
- Structure of 2MASS edge-on galaxies
- Short Name:
- J/ApJ/702/1567
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present results of an analysis of the J, H, and Ks Two Micron All Sky Survey (2MASS) images of 139 spiral edge-on galaxies selected from the Revised Flat Galaxies Catalog. The basic structural parameters scale length (h), scale height (z_0_), and central surface brightness of the stellar disks ({mu}_0_) are determined for all selected galaxies in the near-infrared (NIR) bands. The mean relative ratios of the scale heights of the thin stellar disks in the J:H:Ks bands are 1.16:1.08:1.00, respectively. Comparing the scale heights obtained from the NIR bands for the same objects, we estimate the scale heights of the thin stellar disks corrected for the internal extinction. We find that the extinction-corrected scale height is, on average, 11% smaller than that in the K band. Using the extinction-corrected structural parameters, we find that the dark-to-luminous mass ratio is, on average, 1.3 for the galaxies in our sample within the framework of a simplified galactic model. The relative thicknesses of the stellar disks z_0_/h correlates with their face-on central surface brightnesses obtained from the 2MASS images. We also find that the scale height of the stellar disks shows no systematic growth with radius in most of our galaxies.
- ID:
- ivo://CDS.VizieR/J/ApJ/659/1176
- Title:
- Study of bars in 180 spiral galaxies
- Short Name:
- J/ApJ/659/1176
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Critical insights on galaxy evolution stem from the study of bars. With the advent of HST surveys that trace bars in the rest-frame optical out to z~1, it is critical to provide a reference baseline for bars at z~0 in the optical band. We present results on bars at z~0 in the optical and NIR based on 180 spirals from OSUBSGS (Eskridge et al., 2002, Cat. J/ApJS/143/73).
- ID:
- ivo://CDS.VizieR/J/other/Ap/54.147
- Title:
- Study of 230 IRAS-FSC galaxies
- Short Name:
- J/other/Ap/54.14
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- From the cross-correlation of the IRAS FSC catalog with the radio FIRST catalog, 230 infrared galaxies were selected having optical classifications and redshifts from SDSS and NED. To understand the nature of these objects we have compared them with a sample of bright ULIRGs with fluxes f>1Jy at 60-micron and with 14 optically faint IRAS FSC galaxies, showing that IRAS galaxies are not always strong infrared sources. We also have calibrated Star Formation Rates based on luminosities of the PAH feature at 7.7-micron and 1.4GHz radio flux densities, which confirmed the consistency between these two SFRs. We have estimated the extinction for our 230 objects using SFRs calibrated from the PAH feature compared to ultraviolet flux, which shows that only 1% of the ultraviolet continuum typically escapes extinction by dust within a starburst. As our 230 galaxies have no spectra available from Spitzer Space Telescope (SST) archive, to estimate the infrared flux at 7.7 (for SB galaxies) or 8.0 (for AGN and composite) micron, we have used the median ratios of the IRAS fluxes at 25-micron to fluxes at 7.7 or 8.0-micron estimated for each 41.0<logL(IR)<41.9, 42.0<logL(IR)<42.9, 43.0<logL(IR)<43.9, 44.0<logL(IR)<44.9, and 45.0<logL(IR)<45.9 luminosity bins, using objects having spectra from SST archive.
- ID:
- ivo://CDS.VizieR/J/MNRAS/439/1648
- Title:
- Subarcsecond mid-infrared atlas of local AGN
- Short Name:
- J/MNRAS/439/1648
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the first subarcsecond-resolution mid-infrared (MIR) atlas of local active galactic nuclei (AGN). Our atlas contains 253 AGN with a median redshift of z=0.016, and includes all publicly available MIR imaging performed to date with ground-based 8-m class telescopes, a total of 895 independent measurements. Of these, more than 60% are published here for the first time. We detect extended nuclear emission in at least 21% of the objects, while another 19% appear clearly point-like, and the remaining objects cannot be constrained. Where present, elongated nuclear emission aligns with the ionization cones in Seyferts. Subarcsecond resolution allows us to isolate the AGN emission on scales of a few tens of parsecs and to obtain nuclear photometry in multiple filters for the objects. Median spectral energy distributions (SEDs) for the different optical AGN types are constructed and individual MIR 12 and 18um continuum luminosities are computed. These range over more than six orders of magnitude. In comparison to the arcsecond-scale MIR emission as probed by Spitzer, the continuum emission is much lower on subarcsecond scales in many cases. The silicate feature strength is similar on both scales and generally appears in emission (absorption) in type I (II) AGN. However, the polycyclic aromatic hydrocarbon emission appears weaker or absent on subarcsecond scales. The differences of the MIR SEDs on both scales are particularly large for AGN/starburst composites and close-by (and weak) AGN. The nucleus dominates over the total emission of the galaxy only at luminosities >~10^44^erg/s. The AGN MIR atlas is well suited not only for detailed investigation of individual sources but also for statistical studies of AGN unification.
- ID:
- ivo://CDS.VizieR/J/MNRAS/453/1079
- Title:
- Sub-mJy radio sources SF properties
- Short Name:
- J/MNRAS/453/1079
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We investigate the star formation properties of ~800 sources detected in one of the deepest radio surveys at 1.4GHz. Our sample spans a wide redshift range (~0.1-4) and about four orders of magnitude in star formation rate (SFR). It includes both star-forming galaxies (SFGs) and active galactic nuclei (AGNs), further divided into radio-quiet (RQ) and radio-loud objects. We compare the SFR derived from the far-infrared luminosity, as traced by Herschel, with the SFR computed from their radio emission. We find that the radio power is a good SFR tracer not only for pure SFGs but also in the host galaxies of RQ AGNs, with no significant deviation with redshift or specific SFR. Moreover, we quantify the contribution of the starburst activity in the SFG population and the occurrence of AGNs in sources with different level of star formation. Finally, we discuss the possibility of using deep radio survey as a tool to study the cosmic star formation history.
- ID:
- ivo://CDS.VizieR/J/ApJ/639/259
- Title:
- Sub-mm clumps in Orion B South molecular cloud
- Short Name:
- J/ApJ/639/259
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present results from a survey of a 1300arcmin^2^ region of the Orion B South molecular cloud, including NGC 2024, NGC 2023, and the Horsehead Nebula (B33), obtained using the Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT). Submillimeter continuum observations at 450 and 850{mu}m are discussed. Using an automated algorithm, 57 discrete emission features ("clumps") are identified in the 850{mu}m map.
- ID:
- ivo://CDS.VizieR/J/A+A/466/1065
- Title:
- submm images of IRAS 05358+3543
- Short Name:
- J/A+A/466/1065
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We study the small-scale structure of massive star-forming regions through interferometric observations in several (sub)mm wavelength bands. These observations resolve multiple sources, yield mass and column density estimates, and give information about the density profiles as well as the dust and temperature properties.
