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14621. Star-Forming Galaxies High-Mass X-Ray Binaries Catalog
ID:
ivo://nasa.heasarc/sfgalhmxb
Title:
Star-Forming Galaxies High-Mass X-Ray Binaries Catalog
Short Name:
SFGALHMXB
Date:
09 May 2025
Publisher:
NASA/GSFC HEASARC
Description:
Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, the authors studied populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, the authors find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, L<sub>X</sub> ~ 2.6 x 10<sup>39</sup> x SFR. However, the scaling relations still bear a rather large dispersion of rms ~ 0.4 dex, which the authors believe is of a physical origin. This table contains the catalog of 1055 compact X-ray sources detected within the D25 ellipse for galaxies of this sample which the authors used to construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(L<sub>X</sub>) ~ 35 - 40 luminosity range with a moderately significant evidence for a break or cut-off at L<sub>X</sub> ~ 10<sup>40</sup> erg/s. As before, the authors did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. In their paper, the authors discuss the implications of their results for the theory of binary evolution. In particular, they estimate the fraction of compact objects that once during their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, f<sub>X</sub> ~ 0.2 x (0.1 Myr/tau<sub>x</sub>), where tau<sub>x</sub> is the life time of the X-ray active phase. This is about 4 orders of magnitude more frequent than in low-mass X-ray binaries (LMXBs). The authors also derive constrains on the mass distribution of the secondary star in HMXBs. Note that, in their paper, the authors estimate that ~ 300 of the 1055 sources are likely to be background AGNs (cosmic X-ray background or CXB sources) and that the majority (<~ 700) of the remaining ~ 750 sources are young HMXB systems associated with star formation in their host galaxies. This table was created by the HEASARC in March 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/419/2095">CDS Catalog J/MNRAS/419/2095</a> file hmxb.dat. This is a service provided by NASA HEASARC .
14622. Star-forming galaxies in ACO 2029
ID:
ivo://CDS.VizieR/J/ApJ/773/86
Title:
Star-forming galaxies in ACO 2029
Short Name:
J/ApJ/773/86
Date:
21 Oct 2021
Publisher:
CDS
Description:
Dense environments are known to quench star formation in galaxies, but it is still unknown what mechanism(s) are directly responsible. In this paper, we study the star formation of galaxies in A2029 and compare it to that of Coma, combining indicators at 24{mu}m, H{alpha}, and UV down to rates of 0.03M_{sun}_/yr. We show that A2029's star-forming galaxies follow the same mass-SFR relation as the field. The Coma cluster, on the other hand, has a population of galaxies with star formation rates (SFRs) significantly lower than the field mass-SFR relation, indicative of galaxies in the process of being quenched. Over half of these galaxies also host active galactic nuclei. Ram-pressure stripping and starvation/strangulation are the most likely mechanisms for suppressing the star formation in these galaxies, but we are unable to disentangle which is dominating. The differences we see between the two clusters' populations of star-forming galaxies may be related to their accretion histories, with A2029 having accreted its star-forming galaxies more recently than Coma. Additionally, many early-type galaxies in A2029 are detected at 24{mu}m and/or in the far-UV, but this emission is not directly related to star formation. Similar galaxies have probably been classified as star forming in previous studies of dense clusters, possibly obscuring some of the effects of the cluster environment on true star-forming galaxies.
14623. Star-forming galaxies in AKARI Deep Field-South
ID:
ivo://CDS.VizieR/J/A+A/562/A15
Title:
Star-forming galaxies in AKARI Deep Field-South
Short Name:
J/A+A/562/A15
Date:
21 Oct 2021
Publisher:
CDS
Description:
The main aim of this work is the characterization of physical properties of galaxies detected in the far infrared (FIR) in the AKARI Deep Field-South (ADF-S) survey. Starting from a catalog of the brightest 1000 ADF-S sources in the WIDE-S (90um) AKARI band, we constructed a subsample of galaxies with spectral coverage from the ultraviolet to the far-infrared. Then, we analyzed the multiwavelength properties of this 90um-selected sample of galaxies. For galaxies without known spectroscopic redshifts we computed photometric redshifts using codes Le PHARE and CIGALE, tested these photometric redshifts using spectroscopic redshifts, and compared the performances of both codes. To test the reliability of parameters obtained by fitting Spectral Energy Distributions, a mock catalogue has been generated. We built a large multiwavelength catalog of more than 500 ADF-S galaxies. We successfully fitted Spectral Energy Distributions of 186 galaxies with {chi}^2^<4, and analyzed the output parameters of the fits. We conclude that our sample consists mostly of nearby actively star-forming galaxies, and all our galaxies have a relatively high metallicity. We estimated photometric redshifts for 113 galaxies from the whole ADF-S sample. Comparing the performance of Le PHARE and CIGALE, we found that CIGALE gives more reliable redshift estimates for our galaxies, which implies that including the IR photometry allows for substantial improvement of photometric redshift estimation.
14624. Star-forming galaxies in near-IR
ID:
ivo://CDS.VizieR/J/MNRAS/435/2861
Title:
Star-forming galaxies in near-IR
Short Name:
J/MNRAS/435/2861
Date:
21 Oct 2021
Publisher:
CDS
Description:
The near-infrared spectral region is becoming a very useful wavelength range to detect and quantify the stellar population of galaxies. Models are developing to predict the contribution of the thermally pulsating stars on the asymptotic giant branch stars that should dominate the near-infrared region (NIR) spectra of populations 0.3 to 2Gyr old. When present in a given stellar population, these stars leave unique signatures that can be used to detect them unambiguously. However, these models have to be tested in a homogeneous data base of star-forming galaxies, to check if the results are consistent with what is found from different wavelength ranges. In this work, we performed stellar population synthesis on the nuclear and extended regions of 23 star-forming galaxies to understand how the star formation tracers in the NIR can be used in practice. The stellar population synthesis shows that for the galaxies with strong emission in the NIR, there is an important fraction of young/intermediate population contributing to the spectra, which is probably the ionization source in these galaxies. Galaxies that had no emission lines measured in the NIR were found to have older average ages and less contribution of young populations. Although the stellar population synthesis method proved to be very effective to find the young ionizing population in these galaxies, no clear correlation between these results and the NIR spectral indexes were found. Thus, we believe that, in practice, the use of these indexes is still very limited due to observational limitations.
14625. Star-forming galaxies in the Coma Cluster
ID:
ivo://CDS.VizieR/J/A+A/303/661
Title:
Star-forming galaxies in the Coma Cluster
Short Name:
J/A+A/303/661
Date:
21 Oct 2021
Publisher:
CDS
Description:
In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.
14626. Star-forming galaxies over 0.35<z<2.25
ID:
ivo://CDS.VizieR/J/A+A/625/A114
Title:
Star-forming galaxies over 0.35<z<2.25
Short Name:
J/A+A/625/A114
Date:
21 Oct 2021
Publisher:
CDS
Description:
To better constrain the physical mechanisms driving star formation, we present the first systematic study of the radio continuum size evolution of star-forming galaxies (SFGs) over the redshift range 0.35<z<2.25. We use the VLA COSMOS 3GHz map (noise rms=2.3Jy/beam, {theta}_beam_=0.75arcsec) to construct a mass-complete sample of 3184 radio-selected SFGs that reside on and above the main-sequence (MS) of SFGs. We constrain the overall extent of star formation activity in galaxies by applying a 2D-Gaussian model to their radio continuum emission. Extensive Monte Carlo simulations are used to validate the robustness of our measurements and characterize the selection function. We find no clear dependence between the radio size and stellar mass, M*, of SFGs with 10.5<log(M*/M_{sun}_)<11.5. Our analysis suggests that MS galaxies are preferentially extended, while SFGs above the MS are always compact. The median effective radius of SFGs on (above) the MS of Reff=1.5+/-0.2(1.0+/-0.2)kpc remains nearly constant with cosmic time; a parametrization of the form Reff{prop.to}(1+z)^alpha^ yields a shallow slope of only alpha=-0.26+/-0.08(0.12+/-0.14) for SFGs on (above) the MS. The size of the stellar component of galaxies is larger than that inferred from radio continuum emission by a factor ~2(1.3) at z=0.5(2), indicating star formation is enhanced at small radii. The galactic-averaged star formation rate surface density ({SIGMA}_SFR_) scales with the distance to the MS, except for a fraction of MS galaxies (~10%) that harbor starburst-like {SIGMA}_SFR_. These "hidden" starbursts might have experienced a compaction phase due to disk instability and/or merger-driven burst of star formation, which may or may not significantly offset a galaxy from the MS. We thus propose to use {SIGMA}_SFR_ and distance to the MS in conjunction to better identify the galaxy population undergoing a starbursting phase.
14627. Star-forming low-mass gal. stellar host
ID:
ivo://CDS.VizieR/J/A+A/632/A15
Title:
Star-forming low-mass gal. stellar host
Short Name:
J/A+A/632/A15
Date:
21 Oct 2021
Publisher:
CDS
Description:
The morphological evolution of star-forming galaxies provides important clues to understand their physical properties, as well as the triggering and quenching mechanisms of star formation. We analyze the morphology of galaxies hosting star-forming events at low redshift (z<0.36). We aim at connecting morphology and star-formation properties of low-mass galaxies (median stellar mass ~10^8.5^M_{sun}_) beyond the local Universe. We use a sample of medium-band selected star-forming galaxies from the GOODS-North field. H images for the sample are created combining both spectral energy distribution fits and HST data. Using them, we mask the star forming regions to obtain an unbiased two-dimensional model of the light distribution of the host galaxies. For this purpose we use PHI, a new Bayesian photometric decomposition code. We applied it independently to 7 HST bands, from the ultraviolet to the near-infrared, assuming a Sersic surface brightness model. Star-forming galaxy hosts show low Sersic index (with median n~0.9), as well as small sizes (median Re~1.6kpc), and negligible change of the parameters with wavelength (except for the axis ratio, which grows with wavelength in 46% of the sample). Using a clustering algorithm, we find two different classes of star-forming galaxies: A more compact, redder, and high-n (class A) and a more extended, bluer and lower-n one (class B). This separation holds across all seven bands analyzed. In addition, we find evidence that the first class is more spheroidal-like (according to the distribution of observed axis ratios). We compute the color gradients of the host galaxies finding that 48% of the objects where the analysis could be performed show negative gradients, and only in 5% they are positive. The host component of low-mass star-forming galaxies at z<0.36 separates into two different classes, similar to what has been found for their higher mass counterparts. The results are consistent with an evolution from class B to class A. Several mechanisms from the literature, like minor and major mergers, and violent disk instability, can explain the physical process behind the likely transition between the classes.
14628. Star-forming potential in the Perseus complex
ID:
ivo://CDS.VizieR/J/AJ/153/214
Title:
Star-forming potential in the Perseus complex
Short Name:
J/AJ/153/214
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the results of our investigation of the star-forming potential in the Perseus star-forming complex. We build on previous starless core, protostellar core, and young stellar object (YSO) catalogs from Spitzer (3.6-70 {mu}m), Herschel (70-500 {mu}m), and SCUBA (850 {mu}m) observations in the literature. We place the cores and YSOs within seven star-forming clumps based on column densities greater than 5x10^21^/cm^2^. We calculate the mean density and free-fall time for 69 starless cores as ~5.55x10^-19^ g/cm^3^ and ~0.1 Myr, respectively, and we estimate the star formation rate for the near future as ~150 M_{sun}_/Myr. According to Bonnor-Ebert stability analysis, we find that majority of starless cores in Perseus are unstable. Broadly, these cores can collapse to form the next generation of stars. We found a relation between starless cores and YSOs, where the numbers of young protostars (Class 0 + Class I) are similar to the numbers of starless cores. This similarity, which shows a one-to-one relation, suggests that these starless cores may form the next generation of stars with approximately the same formation rate as the current generation, as identified by the Class 0 and Class I protostars. It follows that if such a relation between starless cores and any YSO stage exists, the SFR values of these two populations must be nearly constant. In brief, we propose that this one-to-one relation is an important factor in better understanding the star formation process within a cloud.
14629. Star Forming Region IRAS12272-6240 JHK photometry
ID:
ivo://CDS.VizieR/J/MNRAS/496/3358
Title:
Star Forming Region IRAS12272-6240 JHK photometry
Short Name:
J/MNRAS/496/3358
Date:
21 Oct 2021
Publisher:
CDS
Description:
IRAS 12272-6240 is a complex star-forming region with a compact massive dense clump (DC) and several associated masers, located at a well-determined distance of d=9.3kpc from the Sun. For this study, we obtained sub-arcsec broad- and narrow-band near-infrared (near-IR) imaging and low-resolution spectroscopy with the Baade/Magellan telescope and its camera PANIC. Mosaics of size 2x2arcmin^2^ in the JHKs bands and with narrow-band filters centred in the 2.12um H_2_ and 2.17um Br{gamma} lines were analysed in combination with Hi-GAL/Herschel and archive IRAC/Spitzer and WISE observations. We found that the compact DC houses two Class I young stellar objects (YSOs) that probably form a 21000-au-wide binary system. Its combined 1-1200um spectral energy distribution is consistent with an O9V central star with a 10^-2^M_{sun}_ disc and a 1.3x10^4^M_{sun}_ dust envelope. Its total luminosity is 8.5x10^4^L_{sun}_. A series of shocked H_2_ emission knots are found in its close vicinity, confirming the presence of outflows. IRAS 12272-6240 is at the centre of an embedded cluster with a mean age of 1Myr and 2.6pc in size that contains more than 150 stars. At its nucleus, we found a more compact and considerably younger subcluster containing the YSOs. We also identified and classified the O-type central stars of two dusty radio/IR HII regions flanking the protostars. Our results confirm that these elements form a single giant young complex where massive star formation processes started some 1Myr ago and are still active.
14630. Star-forming regions deuteration
ID:
ivo://CDS.VizieR/J/A+A/579/A80
Title:
Star-forming regions deuteration
Short Name:
J/A+A/579/A80
Date:
21 Oct 2021
Publisher:
CDS
Description:
The chemical evolution in high-mass star-forming regions is still poorly constrained. Studying the evolution of deuterated molecules allows distinguishing between subsequent stages of high-mass star formation regions based on the strong temperature dependence of deuterium isotopic fractionation. We observed a sample of 59 sources including 19 infrared dark clouds, 20 high-mass protostellar objects, 11 hot molecular cores and 9 ultra-compact HII regions in the (3-2) transitions of the four deuterated molecules, DCN, DNC, DCO^+^, and N_2_D^+^ as well as their non-deuterated counterparts. The overall detection fraction of DCN, DNC, and DCO^+^ is high and exceeds 50% for most of the stages. N_2_D^+^ was only detected in a few infrared dark clouds and high-mass protostellar objects. This may be related to problems in the bandpass at the transition frequency and to low abundances in the more evolved, warmer stages. We find median D/H ratios of 0.02 for DCN, 0.005 for DNC, 0.0025 for DCO^+^, and 0.02 for N_2_D^+^. While the D/H ratios of DNC, DCO^+^, and N_2_D^+^ decrease with time, DCN/HCN peaks at the hot molecular core stage. We only found weak correlations of the D/H ratios for N_2_D^+^ with the luminosity of the central source and the FWHM of the line, and no correlation with the H_2_ column density. In combination with a previously observed set of 14 other molecules (Paper I), we fitted the calculated column densities with an elaborate 1D physico-chemical model with time-dependent D-chemistry including ortho- and para-H_2_ states. Good overall fits to the observed data were obtained with the model. This is one of the first times that observations and modeling were combined to derive chemically based best-fit models for the evolution of high-mass star formation including deuteration.

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