- ID:
- ivo://CDS.VizieR/J/ApJ/731/120
- Title:
- Intrinsic SN Ia light curves
- Short Name:
- J/ApJ/731/120
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have constructed a comprehensive statistical model for Type Ia supernova (SN Ia) light curves spanning optical through near-infrared (NIR) data. A hierarchical framework coherently models multiple random and uncertain effects, including intrinsic supernova (SN) light curve covariances, dust extinction and reddening, and distances. An improved BayeSN Markov Chain Monte Carlo code computes probabilistic inferences for the hierarchical model by sampling the global probability density of parameters describing individual SNe and the population. We have applied this hierarchical model to optical and NIR data of 127 SNe Ia from PAIRITEL, CfA3, Carnegie Supernova Project, and the literature. We find an apparent population correlation between the host galaxy extinction AV and the ratio of total-to-selective dust absorption RV. For SNe with low dust extinction, A_V_<~0.4, we find R_V_~2.5-2.9, while at high extinctions, A_V_>~1, low values of R_V_<2 are favored. The NIR luminosities are excellent standard candles and are less sensitive to dust extinction. They exhibit low correlation with optical peak luminosities, and thus provide independent information on distances. The combination of NIR and optical data constrains the dust extinction and improves the predictive precision of individual SN Ia distances by about 60%. Using cross-validation, we estimate an rms distance modulus prediction error of 0.11mag for SNe with optical and NIR data versus 0.15mag for SNe with optical data alone. Continued study of SNe Ia in the NIR is important for improving their utility as precise and accurate cosmological distance indicators.
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Search Results
- ID:
- ivo://CDS.VizieR/J/ApJ/842/121
- Title:
- Investigating Tully-Fisher relation with KMOS^3D^
- Short Name:
- J/ApJ/842/121
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We investigate the stellar mass and baryonic mass Tully-Fisher relations (TFRs) of massive star-forming disk galaxies at redshift z~2.3 and z~0.9 as part of the KMOS^3D^ integral field spectroscopy survey. Our spatially resolved data allow reliable modeling of individual galaxies, including the effect of pressure support on the inferred gravitational potential. At fixed circular velocity, we find higher baryonic masses and similar stellar masses at z~2.3 as compared to z~0.9. Together with the decreasing gas-to-stellar mass ratios with decreasing redshift, this implies that the contribution of dark matter to the dynamical mass on the galaxy scale increases toward lower redshift. A comparison to local relations reveals a negative evolution of the stellar and baryonic TFR zero points from z=0 to z~0.9, no evolution of the stellar TFR zero point from z~0.9 to z~2.3, and a positive evolution of the baryonic TFR zero point from z~0.9 to z~2.3. We discuss a toy model of disk galaxy evolution to explain the observed nonmonotonic TFR evolution, taking into account the empirically motivated redshift dependencies of galactic gas fractions and the relative amount of baryons to dark matter on galaxy and halo scales.
- ID:
- ivo://CDS.VizieR/J/A+A/659/A131
- Title:
- Ionized Gas Kinematics in MaNGA AGN
- Short Name:
- J/A+A/659/A131
- Date:
- 17 Mar 2022 00:05:59
- Publisher:
- CDS
- Description:
- Feedback from active galactic nuclei (AGN) in general seems to play an important role in the evolution of galaxies, although the impact of AGN winds on their host galaxies is still pending on detailed analysis. We analyse the kinematics of a sample of 170 AGN host galaxies as compared to those of a matched control sample of nonactive galaxies from the MaNGA survey in order to characterise and estimate the extents of the Narrow Line Region (NLR) and of the kinematically disturbed region (KDR) by the AGN. We define the observed NLR radius (r_NLR,o_) as the farthest distance from the nucleus within which both [OIII]/H{beta} and [NII]/H{alpha} ratios fall in the AGN region of the BPT diagram and the H equivalent width is required to be larger than 3.0{AA}. The extent of the KDR (rKDR,o) is defined as the distance from the nucleus within which the AGN hosts galaxies shows a more disturbed gas kinematics than the control galaxies. The AGN [OIII]5007 luminosity ranges from 10^39^ to 10^41^erg/s, and the kinematics derived from the [OIII] line profiles reveal that, on average, the most luminous AGN (L[OIII]>3.8x10^40^erg/s) possess higher residual difference between the gaseous and stellar velocities and velocities dispersion than their control galaxies in all the radial bins. Spatially resolved NLR's and KDR's were found in 55 and 46 AGN host galaxies, with corrected radii 0.2<r_KDR,c_<2.3kpc and 0.4<r_NLR,c_<10.1kpc, with a relation between the two given by logr_KDR,c_=(0.53+/-0.12)logr_NLR,c_+(1.07+/-0.22), respectively. On average, the extension of the KDR corresponds to about 30 per cent of that of the NLR. Assuming that the KDR is due to an AGN outflow, we have estimated ionised gas mass outflow rates that range between 10^-5^ and ~1M_{sun}_/yr, and kinetic powers that range from 10^34^ to 10^40^erg/s. Comparing the power of the AGN ionised outflows with the AGN luminosities, they are always below the 0.05 LAGN model threshold for having a an important feedback effect on their respective host galaxies. The mass outflow rates (and power) of our AGN sample correlate with their luminosities, populating the lowest AGN luminosity range of the correlations previously found for more powerful sources.
- ID:
- ivo://CDS.VizieR/J/AJ/159/216
- Title:
- Ions density in the CGM of low mass galaxy groups
- Short Name:
- J/AJ/159/216
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We explore how environment affects the metallicity of the circumgalactic medium (CGM) using 13 low-mass galaxy groups (two to five galaxies) at <z_abs_>=0.25 identified near background quasars. Using quasar spectra from the Hubble Space Telescope/Cosmic Origins Spectrograph (HST/COS) and from Keck/High Resolution Echelle Spectrometer (Keck/HIRES) or the Very Large Telescope/Ultraviolet and Visual Echelle Spectrograph (VLT/UVES), we measure column densities of or determine limits on CGM absorption lines. We use a Markov Chain Monte Carlo approach with Cloudy to estimate metallicities of cool (T~104K) CGM gas within groups and compare them to CGM metallicities of 47 isolated galaxies. Both group and isolated CGM metallicities span a wide range (-2<[Si/H]<0), where the mean group (-0.54{pm}0.22) and isolated (-0.77{pm}0.14) CGM metallicities are similar. Group and isolated environments have similar distributions of HI column densities as a function of impact parameter. However, contrary to isolated galaxies, we do not find an anticorrelation between HI column density and the nearest group galaxy impact parameter. We additionally divided the groups by member luminosity ratios (i.e., galaxy-galaxy and galaxy-dwarf groups). While there was no significant difference in their mean metallicities, a modest increase in sample size should allow one to statistically identify a higher CGM metallicity in galaxy-dwarf groups compared to galaxy-galaxy groups. We conclude that either environmental effects have not played an important role in the metallicity of the CGM at this stage and expect that this may only occur when galaxies are strongly interacting or merging or that some isolated galaxies have higher CGM metallicities due to past interactions. Thus, environment does not seem to be the cause of the CGM metallicity bimodality.
- ID:
- ivo://CDS.VizieR/J/ApJ/756/72
- Title:
- IRAC identifications for 510 AEGIS20 radio sources
- Short Name:
- J/ApJ/756/72
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Infrared 3.6-8{mu}m images of the Extended Groth Strip yield plausible counterpart identifications for all but one of 510 radio sources in the AEGIS20 S(1.4GHz)>50{mu}Jy sample. This is the first such deep sample that has been effectively 100% identified. Achieving the same identification rate at R band would require observations reaching R_AB_>27. Spectroscopic redshifts are available for 46% of the sample and photometric redshifts for an additional 47%. Almost all of the sources with 3.6{mu}m AB magnitudes brighter than 19 have spectroscopic redshifts z<1.1, while fainter objects predominantly have photometric redshifts with 1<~z<~3. Unlike more powerful radio sources that are hosted by galaxies having large stellar masses within a relatively narrow range, the AEGIS20 counterparts have stellar masses spanning more than a factor of 10 at z~1. The sources are roughly 10%-15% starbursts at z<~0.5 and 20%-25% active galactic nuclei mostly at z>1 with the remainder of uncertain nature.
- ID:
- ivo://CDS.VizieR/J/AJ/110/1993
- Title:
- IRAS Bright Galaxy Survey. II
- Short Name:
- J/AJ/110/1993
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities >5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec<~-30deg, and low Galactic latitudes, 5deg<|b|<=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z<~0.1) Universe.
- ID:
- ivo://CDS.VizieR/J/A+A/299/347
- Title:
- IRAS galaxies behind Taurus clouds
- Short Name:
- J/A+A/299/347
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We carried out a complete search for IRAS galaxies in the Taurus molecular cloud region at l=169deg to 177deg and b=-19deg to -12deg. We selected a total number of 36 galaxies and galaxy candidates and looked for the 21-cm H I line in 25 objects; we detected H I emission in five of them including one with previously unknown redshift. The spatial density of IRAS galaxies with cz=4000 to 6000km/s is lower in this region than in the adjacent regions at both sides along galactic longitude, where the Perseus supercluster and the Gemini-Monoceros filament are respectively located.
- ID:
- ivo://CDS.VizieR/J/AJ/126/1607
- Title:
- IRAS Revised Bright Galaxy Sample
- Short Name:
- J/AJ/126/1607
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- IRAS flux densities, redshifts, and infrared luminosities are reported for all sources identified in the IRAS Revised Bright Galaxy Sample (RBGS), a complete flux-limited survey of all extragalactic objects with total 60{mu}m flux density greater than 5.24Jy, covering the entire sky surveyed by IRAS at Galactic latitudes |b|>5{deg}. The RBGS includes 629 objects, with median and mean sample redshifts of 0.0082 and 0.0126, respectively, and a maximum redshift of 0.0876. The RBGS supersedes the previous two-part IRAS Bright Galaxy Samples (BGS1+BGS2) which were compiled before the final (Pass 3) calibration of the IRAS Level 1 Archive in 1990 May.
- ID:
- ivo://CDS.VizieR/J/ApJ/876/132
- Title:
- IR-bright DOGs viewed with Subaru HSC
- Short Name:
- J/ApJ/876/132
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report on the optical properties of infrared (IR)-bright dust-obscured galaxies (DOGs) that are defined as (i-[22])_AB_>=7.0. Because supermassive black holes (SMBHs) in IR-bright DOGs are expected to be rapidly growing in the major-merger scenario, they provide useful clues for understanding the coevolution of SMBHs and their host galaxies. However, the optical properties of IR-bright DOGs remain unclear because the optical emission of a DOG is very faint. By combining ~105deg^2^ images of the optical, near-IR, and mid-IR data obtained from the Subaru Hyper Suprime-Cam (HSC) survey, the VISTA VIKING survey, and the Wide-field Infrared Survey Explorer all-sky survey, respectively, 571 IR-bright DOGs were selected. We found that IR-bright DOGs show a redder (g-z)_AB_ color than do other populations of dusty galaxies, such as ultraluminous IR galaxies (ULIRGs) at a similar redshift, with a significantly large dispersion. Among the selected DOGs, star formation (SF)-dominated DOGs show a relatively red color, while active galactic nucleus (AGN)-dominated DOGs show a rather blue color in optical. This result is consistent with the idea that the relative AGN contribution in the optical emission becomes more significant at a later stage in the major-merger scenario. We discovered eight IR-bright DOGs showing a significant blue excess in blue HSC bands. This blue excess can be interpreted as a leaked AGN emission that is either a directly leaking or a scattered AGN emission, as proposed for some blue-excess Hot DOGs in earlier studies.
- ID:
- ivo://CDS.VizieR/J/ApJ/756/28
- Title:
- IR counterparts to submm H-ATLAS galaxies
- Short Name:
- J/ApJ/756/28
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We use Spitzer-IRAC data to identify near-infrared counterparts to submillimeter galaxies detected with Herschel-SPIRE at 250{mu}m in the Herschel Astrophysical Terahertz Large Area Survey. Using a likelihood ratio analysis we identify 146 reliable IRAC counterparts to 123 SPIRE sources out of the 159 in the survey area. We find that, compared to the field population, the SPIRE counterparts occupy a distinct region of the 3.6 and 4.5{mu}m color-magnitude space, and we use this property to identify 23 further counterparts to 13 SPIRE sources. The IRAC identification rate of 86% is significantly higher than those that have been demonstrated with wide-field ground-based optical and near-IR imaging of Herschel fields. We estimate a false identification rate of 3.6%, corresponding to 4-5 sources. Among the 73 counterparts that are undetected in Sloan Digital Sky Survey, 57 have both 3.6 and 4.5{mu}m coverage. Of these, 43 have [3.6]-[4.5]>0, indicating that they are likely to be at z>~1.4. Thus, ~40% of identified SPIRE galaxies are likely to be high-redshift (z>~1.4) sources. We discuss the statistical properties of the IRAC-identified SPIRE galaxy sample including far-IR luminosities, dust temperatures, star formation rates, and stellar masses. The majority of our detected galaxies have 10^10^-10^11^L_{sun}_ total IR luminosities and are not intense starbursting galaxies as those found at z~2, but they have a factor of 2-3 above average specific star formation rates compared to near-IR selected galaxy samples.
