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2372. 500{mu}m-risers sources
- ID:
- ivo://CDS.VizieR/J/A+A/614/A33
- Title:
- 500{mu}m-risers sources
- Short Name:
- J/A+A/614/A33
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Context. Over the last decade a large number of dusty star-forming galaxies has been discovered up to redshift z=2-3 and recent studies have attempted to push the highly confused Herschel SPIRE surveys beyond that distance. To search for z>=4 galaxies they often consider the sources with fluxes rising from 250{mu}m to 500{mu}m (so-called "500{mu}m-risers"). Herschel surveys offer a unique opportunity to efficiently select a large number of these rare objects, and thus gain insight into the prodigious star-forming activity that takes place in the very distant Universe. Aims. We aim to implement a novel method to obtain a statistical sample of 500{mu}m-risers and fully evaluate our selection inspecting different models of galaxy evolution. Methods. We consider one of the largest and deepest Herschel surveys, the Herschel Virgo Cluster Survey. We develop a novel selection algorithm which links the source extraction and spectral energy distribution fitting. To fully quantify selection biases we make end-to-end simulations including clustering and lensing. Results. We select 133 500{mu}m-risers over 55deg^2^, imposing the criteria: S_500_>S_350_>S_250_, S_250_>13.2mJy and S_500_>30mJy. Differential number counts are in fairly good agreement with models, displaying a better match than other existing samples. The estimated fraction of strongly lensed sources is 24_+6_^-5^% based on models.Conclusions. We present the faintest sample of 500{mu}m-risers down to S_250_=13.2mJy. We show that noise and strong lensing have an important impact on measured counts and redshift distribution of selected sources. We estimate the flux-corrected star formation rate density at 4<z<5 with the 500{mu}m-risers and find it to be close to the total value measured in far-infrared. This indicates that colour selection is not a limiting effect to search for the most massive, dusty z>4 sources.
- ID:
- ivo://CDS.VizieR/J/ApJ/634/L1
- Title:
- 16{mu}m sources in the NOAO Bootes field
- Short Name:
- J/ApJ/634/L1
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using the 16{mu}m peak-up imager on the Infrared Spectrograph (IRS) on Spitzer, we present a serendipitous survey of 0.0392{deg}^2^ within the area of the NOAO Deep Wide-Field Survey in Bootes. Combining our results with the available Multiband Imaging Photometer for Spitzer (MIPS) 24{mu}m survey of this area, we produce a catalog of 150 16{mu}m sources brighter than 0.18mJy (3{sigma}) for which we derive measures or limits on the 16{mu}m/24{mu}m colors. Such colors are especially useful in determining redshifts for sources whose mid-infrared spectra contain strong emission or absorption features that characterize these colors as a function of redshift.
- ID:
- ivo://CDS.VizieR/J/A+A/654/A80
- Title:
- MUSE Catalog of UV emission line measurement
- Short Name:
- J/A+A/654/A80
- Date:
- 02 Feb 2022 10:08:10
- Publisher:
- CDS
- Description:
- Rest-frame ultraviolet (UV) emission lines probe electron densities, gas-phase abundances, metallicities, and ionization parameters of the emitting star-forming galaxies and their environments. The strongest main UV emission line, Ly{alpha}, has been instrumental in advancing the general knowledge of galaxy formation in the early universe. However, observing Ly{alpha} emission becomes increasingly challenging at z>~6 when the neutral hydrogen fraction of the circumgalactic and intergalactic media increases. Secondary weaker UV emission lines provide important alternative methods for studying galaxy properties at high redshift. We present a large sample of rest-frame UV emission line sources at intermediate redshift for calibrating and exploring the connection between secondary UV lines and the emitting galaxies' physical properties and their Ly{alpha} emission. The sample of 2052 emission line sources with 1.5<z<6.4 was collected from integral field data from the MUSE-Wide and MUSE-Deep surveys taken as part of Guaranteed Time Observations. The objects were selected through untargeted source detection (i.e., no preselection of sources as in dedicated spectroscopic campaigns) in the three-dimensional MUSE data cubes. We searched optimally extracted one-dimensional spectra of the full sample for UV emission features via emission line template matching, resulting in a sample of more than 100 rest-frame UV emission line detections. We show that the detection efficiency of (non-Ly{alpha}) UV emission lines increases with survey depth, and that the emission line strength of HeII {lambda}1640AA, [OIII] {lambda}1661 + OIII] {lambda}1666, and [SiIII] {lambda}1883 + SiIII] {lambda}1892 correlate with the strength of [CIII] {lambda}1907 + CIII] {lambda}1909. The rest-frame equivalent width (EW0 ) of [CIII] {lambda}1907+CIII] {lambda}1909 is found to be roughly 0.22+/-0.18 of EW0 (Ly{alpha}). We measured the velocity offsets of resonant emission lines with respect to systemic tracers. For CIV {lambda}1548 + CIV {lambda}1551 we find that {DELTA}v_CIV_<~250km/s, whereas {nu}v_Ly{alpha}_ falls in the range of 250-500km/s which is in agreement with previous results from the literature. The electron density ne measured from [SiIII] {lambda}1883 + SiIII] {lambda}1892 and [CIII] {lambda}1907 + CIII] {lambda}1909 line flux ratios is generally <10^5^cm^-3^ and the gas-phase abundance is below solar at 12+log10(O/H)~=8. Lastly, we used "PhotoIonization Model Probability Density Functions" to infer physical parameters of the full sample and individual systems based on photoionization model parameter grids and observational constraints from our UV emission line searches. This reveals that the UV line emitters generally have ionization parameter log10(U) ~= -2.5 and metal mass fractions that scatter around Z~=10-2, that is Z~=0.66Z_{sun}_. Value-added catalogs of the full sample of MUSE objects studied in this work (this catalog) and a collection of UV line emitters from the literature are provided with this paper.
- ID:
- ivo://CDS.VizieR/J/A+A/609/A78
- Title:
- MUSE combined data cubes for NGC 3311
- Short Name:
- J/A+A/609/A78
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Early-type galaxies (ETGs) show a strong size evolution with redshift. This evolution is explained by fast "in-situ" star formation at high-z followed by a late mass assembly mostly driven by minor mergers that deposit stars primarily in the outer halo. Aims: We aim to identify the main structural components of the Hydra I cD galaxy NGC 3311 to investigate the connection between the central galaxy and the surrounding stellar halo. We produce maps of the line-of-sight velocity distribution (LOSVD) moments from a mosaic of MUSE pointings covering NGC 3311 out to 25kpc. Combining deep photometric and spectroscopic data, we model the LOSVD maps using a finite mixture distribution, including four non-concentric components that are nearly isothermal spheroids, with different line-of-sight systemic velocities V, velocity dispersions sigma, and small (constant) values of the higher order Gauss-Hermite moments h_3_ and h_4_. The kinemetry analysis indicates that NGC 3311 is classified as a slow rotator, although the galaxy shows a line-of-sight velocity gradient along the photometric major axis. The comparison of the correlations between h_3_ and h_4_ with V{sigma} with simulated galaxies indicates that NGC 3311 assembled mainly through dry mergers. The sigma profile rises to approximately 400$ km/s at 20kpc, a significant fraction (0.55) of the Hydra I cluster velocity dispersion, indicating that stars there were stripped from progenitors orbiting in the cluster core. The finite mixture distribution modeling supports three inner components related to the central galaxy and a fourth component with large effective radius (51kpc) and velocity dispersion (327km/s) consistent with a cD envelope. We find that the cD envelope is offset from the center of NGC 3311 both spatially (8.6kpc) and in velocity ({delta}V=204km/s), but coincides with the cluster core X-ray isophotes and the mean velocity of core galaxies. Also, the envelope contributes to the broad wings of the LOSVD measured by large h_4 values within 10 kpc. The cD envelope of NGC 3311 is dynamically associated with the cluster core, which in Hydra I is in addition displaced from the cluster center, presumably due to a recent subcluster merger.
2376. MUSE datacube of He 2-10
- ID:
- ivo://CDS.VizieR/J/A+A/604/A101
- Title:
- MUSE datacube of He 2-10
- Short Name:
- J/A+A/604/A101
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We study the physical and dynamical properties of the ionized gas in the prototypical HII galaxy Henize 2-10 using MUSE integral field spectroscopy. The large-scale dynamics are dominated by extended outflowing bubbles that are probably the result of massive gas ejection from the central star forming regions. We derived a mass outflow rate dM_out_/dt~0.30M_{sun}_/yr, corresponding to mass loading factor {eta}~0.4, in the range of similar measurements in local LIRGs. Such a massive outflow has a total kinetic energy that is sustainable by the stellar winds and supernova remnants expected in the galaxy. We studied the dust extinction, electron density, and ionization conditions all across the galaxy with a classical emission line diagnostic, confirming the extreme nature of the highly star forming knots in the core of the galaxy, which show high density and high ionization parameters. We measured the gas-phase metallicity in the galaxy, taking the strong variation of the ionization parameter into account, and found that the external parts of the galaxy have abundances as low as 12+log(O/H)~8.3, while the central star forming knots are highly enriched with super solar metallicity. We found no sign of AGN ionization in the galaxy, despite the recent claim of the presence of a supermassive active black hole in the core of He 2-10. We therefore reanalyzed the X-ray data that were used to propose the presence of the AGN, but we concluded that the observed X-ray emission can be better explained with sources of a different nature, such as a supernova remnant.
- ID:
- ivo://CDS.VizieR/J/A+A/625/A102
- Title:
- MUSE datacube of MRC 0943-242
- Short Name:
- J/A+A/625/A102
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have used the Multi-Unit Spectroscopic Explorer (MUSE) to study the circumgalactic medium (CGM) of a z=2.92 radio galaxy, MRC 0943-242 by parametrising its emitting and absorbing gas. In both Ly{alpha} {lambda}1216 and HeII {lambda}1640 lines, we observe emission with velocity shifts of {Delta}v=~-1000km/s from the systemic redshift of the galaxy. These blueshifted components represent kinematically perturbed gas that is aligned with the radio axis, which we interpret as jet-driven outflows. Three of the four known Ly absorbers are detected at the same velocity as CIV {lambda}{lambda}1548,1551 and NV {lambda}{lambda}1239,1243 absorbers, proving that the gas is metal-enriched more so than previously thought. At the velocity of a strong Ly{alpha} absorber with an HI column of N_HI_/cm^-2^=10^19.2^ and velocity shift of Delta}v=~-400km/s, we also detect SiII {lambda}1260 and SiII {lambda}1527 absorption, which suggests that the absorbing gas is ionisation bounded. With the added sensitivity of this MUSE observation, we are more capable of adding constraints to absorber column densities and consequently determining what powers their ionisation. To do this, we obtain photoionisation grid models in cloudy which show that AGN radiation is capable of ionising the gas and producing the observed column densities in a gas of metallicity of Z/Z_{sun}_~=0.01 with a nitrogen abundance a factor of 10 greater than that of hydrogen. This metal-enriched absorbing gas, which is also spatially extended over a projected distance of r>~60kpc, is likely to have undergone chemical enrichment through stellar winds that have swept up metals from the interstellar-medium and deposited them in the outer regions of the galaxy's halo.
- ID:
- ivo://CDS.VizieR/J/A+A/644/A15
- Title:
- MUSE data for MR 2251-178 and PG 1126-041
- Short Name:
- J/A+A/644/A15
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We use MUSE adaptive optics (AO) data in Narrow Field Mode to study the properties of the ionised gas in MR 2251-178 and PG 1126-041, two nearby (z~0.06) bright quasars hosting sub-pc scale Ultra Fast Outflows (UFOs) detected in the X-ray band. We decompose the optical emission from diffuse gas into a low- and a high-velocity components. The former is characterised by a clean, regular velocity field and a low (~80 km/s) velocity dispersion. It traces regularly rotating gas in PG 1126-041, while in MR 2251-178 it is possibly associated to tidal debris from a recent merger or flyby. The other component is found to be extended up to a few kpc from the nuclei, and shows a high (~800km/s) velocity dispersion and a blue-shifted mean velocity, as expected from AGN-driven outflows. We estimate mass outflow rates up to a few Mo/yr and kinetic efficiencies between 0.1-0.4 per cent, in line with those of galaxies hosting AGNs of similar luminosity. The momentum rates of these ionised outflows are comparable to those measured for the UFOs at sub-pc scales, consistent with a momentum-driven wind propagation. Pure energy-driven winds are excluded unless about 100x additional momentum is locked in massive molecular winds. By comparing the outflow properties of our sources with those of a small sample of well-studied QSOs hosting UFOs from the literature, we find that winds seem to systematically lie either in a momentum-driven or in an energy-driven regime, indicating that these two theoretical models bracket very well the physics of AGN-driven winds.
2379. MUSE 3D view of HDF-S
- ID:
- ivo://CDS.VizieR/J/A+A/575/A75
- Title:
- MUSE 3D view of HDF-S
- Short Name:
- J/A+A/575/A75
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We observed Hubble Deep Field South with the new panoramic integral-field spectrograph MUSE that we built and have just commissioned at the VLT. The data cube resulting from 27h of integration covers one arcmin^2^ field of view at an unprecedented depth with a 1{sigma} emission-line surface brightness limit of 1x10^-19^erg/s/cm2/arcsec2, and contains ~90000 spectra. We present the combined and calibrated data cube, and we performed a first-pass analysis of the sources detected in the Hubble Deep Field South imaging. We measured the redshifts of 189 sources up to a magnitude I_814_=29.5, increasing the number of known spectroscopic redshifts in this field by more than an order of magnitude. We also discovered 26 Ly{alpha} emitting galaxies that are not detected in the HST WFPC2 deep broad-band images. The intermediate spectral resolution of 2.3{AA} allows us to separate resolved asymmetric Ly{alpha} emitters, [OII]3727 emitters, and [CIII]1908 emitters, and the broad instantaneous wavelength range of 4500{AA} helps to identify single emission lines, such as [OIII]5007, H{beta}, and H{alpha}, over a very wide redshift range. We also show how the three-dimensional information of MUSE helps to resolve sources that are confused at ground-based image quality. Overall, secure identifications are provided for 83% of the 227 emission line sources detected in the MUSE data cube and for 32% of the 586 sources identified in the HST catalogue. The overall redshift distribution is fairly flat to z=6.3, with a reduction between z=1.5 to 2.9, in the well-known redshift desert. The field of view of MUSE also allowed us to detect 17 groups within the field. We checked that the number counts of [OII]3727 and Ly{alpha} emitters are roughly consistent with predictions from the literature. Using two examples, we demonstrate that MUSE is able to provide exquisite spatially resolved spectroscopic information on the intermediate-redshift galaxies present in the field. This unique data set can be used for a wide range of follow-up studies. We release the data cube, the associated products, and the source catalogue with redshifts, spectra, and emission-line fluxes.
- ID:
- ivo://CDS.VizieR/J/A+A/608/A2
- Title:
- MUSE Hubble Ultra Deep Field Survey. II.
- Short Name:
- J/A+A/608/A2
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have conducted a two-layered spectroscopic survey (1'x1' ultra deep and 3'x3'deep regions) in the Hubble Ultra Deep Field (HUDF) with the Multi Unit Spectroscopic Explorer (MUSE). The combination of a large field of view, high sensitivity, and wide wavelength coverage provides an order of magnitude improvement in spectroscopically confirmed redshifts in the HUDF; i.e., 1206 secure spectroscopic redshifts for Hubble Space Telescope (HST) continuum selected objects, which corresponds to 15% of the total (7904). The redshift distribution extends well beyond z>3 and to HST/F775W magnitudes as faint as ~=30mag (AB, 1{sigma}). In addition, 132 secure redshifts were obtained for sources with no HST counterparts that were discovered in the MUSE data cubes by a blind search for emission-line features. In total, we present 1338 high quality redshifts, which is a factor of eight increase compared with the previously known spectroscopic redshifts in the same field. We assessed redshifts mainly with the spectral features [OII] at z<1.5 (473 objects) and Ly{alpha} at 2.9<z<6.7 (692 objects). With respect to F775W magnitude, a 50% completeness is reached at 26.5mag for ultra deep and 25.5mag for deep fields, and the completeness remains >=20% up to 28-29mag and ~=27mag, respectively. We used the determined redshifts to test continuum color selection (dropout) diagrams of high-z galaxies. The selection condition for F336W dropouts successfully captures ~=80% of the targeted z~2.7 galaxies. However, for higher redshift selections (F435W, F606W, and F775W dropouts), the success rates decrease to ~=20-40%. We empirically redefine the selection boundaries to make an attempt to improve them to ~=60%. The revised boundaries allow bluer colors that capture Ly{alpha} emitters with high Ly{alpha} equivalent widths falling in the broadbands used for the color-color selection. Along with this paper, we release the redshift and line flux catalog.
