- ID:
- ivo://CDS.VizieR/J/AJ/112/359
- Title:
- Galaxies in the Hubble Deep Field
- Short Name:
- J/AJ/112/359
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a catalog of morphological and color data for galaxies with 21<I_814<25mag in the Hubble Deep Field (Williams et al. 1996, in Science with the Hubble Space Telescope II). Galaxies have been inspected and (when possible) independently visually classified on the MDS and DDO systems. Measurements of central concentration and asymmetry are also included in the catalog. The fraction of interacting and merging objects is seen to be significantly higher in the Hubble Deep Field than it is among nearby galaxies. Barred spirals are essentially absent from the deep sample. The fraction of early-type galaxies in the Hubble Deep Field is similar to the fraction of early-types in the Shapley-Ames Catalog, but the fraction of galaxies resembling archetypal grand-design late-type spiral galaxies is dramatically lower in the distant HDF sample.
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Search Results
- ID:
- ivo://CDS.VizieR/J/AJ/132/926
- Title:
- Galaxies in the Hubble Ultra Deep Field
- Short Name:
- J/AJ/132/926
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present aperture-matched point-spread function (PSF)corrected BVi'z'JH photometry and Bayesian photometric redshifts (BPZ) for objects detected in the Hubble Ultra Deep Field (UDF), 8042 of which are detected at the 10 level (e.g., i'<29.01 or z'<28.43). Most of our objects are defined identically to those in the public STScI catalogs, enabling a straightforward object-by-object comparison. We have combined detections from i', z', J+H, and B+V+i'+ z' images into a single comprehensive segmentation map. Using a new program called SExSeg, we are able to force this segmentation map into SExtractor for photometric analysis. The resulting photometry is corrected for the wider NIC3 PSFs using our ColorPro software. We also correct for the ACS z'-band PSF halo. Offsets are applied to our NIC3 magnitudes, which are found to be too faint relative to the ACS fluxes. Based on BPZ spectral energy distribution (SED) fits to objects of known spectroscopic redshift, we derived corrections of -0.30+/-0.03mag in J and -0.18+/-0.04mag in H. Our offsets appear to be supported by a recent recalibration of the UDF NIC3 images combined with nonlinearity measured in NICMOS itself. The UDF reveals a large population of faint blue galaxies (presumably young starbursts), bluer than those observed in the original Hubble Deep Fields.
- ID:
- ivo://CDS.VizieR/J/MNRAS/415/1188
- Title:
- Galaxies in the Lynx-Cancer void
- Short Name:
- J/MNRAS/415/1188
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The evolution of galaxies is influenced by the environment in which they reside. This effect should be strongest for the lowest-mass and lowest-luminosity galaxies. To study dwarf galaxies in extremely low density environments, we have compiled a deep catalogue of dwarf galaxies in the nearby Lynx-Cancer void. This void hosts some of the most metal-poor dwarfs known to date. It borders the Local Volume at negative supergalactic Z(SGZ) coordinates and has a size of more than 16Mpc. With a distance to its centre of only 18Mpc, it is close enough to allow a search for the faintest dwarfs. Within the void 75 dwarf (-11.9>M_B_>-18.0) and four subluminous (-18.0>M_B_>-18.4) galaxies have been identified. We present the parameters of the void galaxies and a detailed analysis of the completeness of the catalogue as a function of magnitude and surface brightness.
- ID:
- ivo://CDS.VizieR/J/A+A/640/A30
- Title:
- Galaxies in the Perseus cluster field
- Short Name:
- J/A+A/640/A30
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We investigate the galaxies brighter than B~20 in the field of the Perseus cluster. The galaxies were selected on Schmidt CCD images in B and Halpha in combination with SDSS images. The survey field roughly covers the virial radius of the cluster. The galaxy sample is used for analysing cluster properties, such as radial profiles, indications of sub-structure, virial mass, and viral radius and is applied for a study of the cluster galaxy population with an emphasis on morphological types and peculiarities, star formation rates and active galactic nuclei.
- ID:
- ivo://CDS.VizieR/J/A+A/413/771
- Title:
- Galaxies in the Tycho-2 catalogue
- Short Name:
- J/A+A/413/771
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The accuracy of the link of the proper motion system of astrometric satellite missions like AMEX and GAIA is discussed. Monte-Carlo methods were used to simulate catalogues of positions and proper motions of quasars and galaxies to test the link. The main conclusion is, that future satellite missions like GAIA may be "self-calibrated" by their measurements of QSOs, while additional measurements from radio stars or HST-data are needed to calibrate the less deep reaching astrometric satellite missions of AMEX type.
- ID:
- ivo://CDS.VizieR/J/MNRAS/429/2264
- Title:
- Galaxies in the UMa cluster complex
- Short Name:
- J/MNRAS/429/2264
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A nearby friable cloud in Ursa Majoris contains 270 galaxies with radial velocities 500<V_LG_<1500km/s inside the area of RA=[11.0h,13.0h] and DE=[+40{deg},+60{deg}]. At present, 97 galaxies of them have individual distance estimates. We use these data to clarify the structure and kinematics of the UMa complex. According to Makarov & Karachentsev (2011MNRAS.412.2498M, Cat. J/MNRAS/412/2498), most of the UMa galaxies belong to seven bound groups, which have the following median parameters: velocity dispersion of 58k/s, harmonic projected radius of 300kpc, virial mass of 2x10^12^M{sun} and virial mass-to-K-band luminosity ratio of 27M{sun}/L{sun}. Almost a half of the UMa cloud population are gas-rich dwarfs (Ir, Im, BCD) with active star formation seen in the GALEX UV-survey. The UMa groups reside within 15-19Mpc from us, being just at the same distance as the Virgo cluster. The total virial mass of the UMa groups is 4x10^13^M{sun}, yielding the average density of dark matter in the UMa cloud to be {Omega}m=0.08, i.e. a factor of 3 lower than the cosmic average. This is despite the fact that the UMa cloud resides in a region of the Universe that is an apparent overdensity. A possible explanation for this is that most mass in the Universe lies in the empty space between clusters. Herewith, the mean distances and velocities of the UMa groups follow nearly undisturbed Hubble flow without a sign of the 'Z-wave' effect caused by infall towards a massive attractor. This constrains the total amount of dark matter between the UMa groups within the cloud volume.
- ID:
- ivo://CDS.VizieR/J/ApJ/449/527
- Title:
- Galaxies in the zone of avoidance
- Short Name:
- J/ApJ/449/527
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have selected a sample of 876 galaxy candidates from the IRAS Point Source Catalog in the region of 2h<RA<10h and 0deg<DE<36deg, which crosses the Galactic anticenter part of the Zone of Avoidance (ZOA) and includes most of the highly obscured Orion-Taurus complex region. We have identified galaxies among the candidate sources by attempting to detect the 21cm H I line of those sources which were not known to be galaxies at the beginning of the survey. In this manner, we constructed a galaxy sample which is largely free from Galactic reddening. Of the 272 observed candidates, 89 were detected in the H I line up to a heliocentric velocity of v_h_~16,000km/s. The resulting galaxy sample of 717 galaxies is fairly complete (within about 10%) and uniform (within about 4%) in the part of the survey area 10deg away from the Galactic plane and for velocities up to at least 9000km/s. This provides, for the first time, a largely unbiased view on the large-scale structures in much of the survey area. Our main results are the following: (1) Several large voids are identified. In particular, a void between RA~3h and 4h, up to v_h_~6000km/s, separates the Pisces-Perseus supercluster at RA<3h from structures at RA>4h; and a "nearby void" occupies most of our survey area and reaches out to a redshift of nearly 3000km/s. (2) We found no nearby galaxy concentration that could significantly contribute to the "Local Velocity Anomaly" (LVA), but a general excess of galaxies around v_h_~5000km/s in the survey area. (3) The contrast between the "Great Wall" at v_h_~8500km/s and the void in front of it appears to gradually diffuse out after it enters the Zone of Avoidance from the northern Galactic hemisphere. (4) Our data combined with other galaxy surveys in or near the Galactic anticenter part of the ZOA suggest that the main ridge of the Pisces-Perseus supercluster does also not extend to Abell 569, a cluster in the northern Galactic hemisphere, and that the simple gravitational model consisting of the Local Void of Tully & Fisher, our nearby void, and Puppis and Fornax-Eridanus clusters would predict a LVA whose direction is probably too far away from that derived from observations.
- ID:
- ivo://CDS.VizieR/J/A+AS/110/269
- Title:
- Galaxies in the "zone of avoidance". I.
- Short Name:
- J/A+AS/110/269
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a compilation of hopefully all published galaxies and quasars that were ever optically identified within |b|=<5deg. We present 2304 objects and list (and discuss), in addition to their (often considerably improved) coordinates, the best available morphological type, optical maximum diameters in the red, up-to-date heliocentric radial velocities, references to the papers where a specific object was first optically identified and results of cross-checks with the IRAS point source catalogue.
- ID:
- ivo://CDS.VizieR/J/A+AS/117/1
- Title:
- Galaxies in the "zone of avoidance". II.
- Short Name:
- J/A+AS/117/1
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg<=b<=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l>=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.
- ID:
- ivo://CDS.VizieR/J/A+AS/117/369
- Title:
- Galaxies in the "zone of avoidance". III.
- Short Name:
- J/A+AS/117/369
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- As the third part in a series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present a compilation of 1161 galaxies discovered during a systematic search on Palomar Observatory Sky Survey (POSS) red-sensitive prints. The region searched comprises 200 square degrees, at 120deg<=l<=130deg, -10deg<=b<=+10deg. In addition to galactic, equatorial and rectangular coordinates, we list maximum and minimum optical diameters derived from both the red- and blue-sensitive prints, could assign a morphological type to some of the objects and made cross-checks with the IRAS PSC and several radio catalogues. A test for completeness suggests, that our catalogue should be complete down to a limiting galaxy-diameter of 0.35'. An asymmetric distribution of the galaxies with respect to the galactic equator was found and is discussed by comparing it with the locations of optically visible dust clouds and/or the distribution of IR-emitting dust material. A comparison between the distribution of the galaxies and the 100{mu} IRAS intensity maps led to the identification of four possible clusterings. As a byproduct of our galaxy search, two new planetary nebulae, nebulous stars at the position of a strong cold IRAS point source, and a nearby dwarf irregular galaxy could be detected.
