- 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.
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Search Results
- ID:
- ivo://CDS.VizieR/J/MNRAS/437/1858
- Title:
- Galaxies in the RX J1347.5-1145 cluster
- Short Name:
- J/MNRAS/437/1858
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a revised strong lensing mass reconstruction of the galaxy cluster RX J1347.5-1145. The X-ray luminous cluster at redshift z=0.451 has already been studied intensively in the past. Based on information of two such previous (strong-) lensing studies by Halkola et al. (2008A&A...481...65H) and Bradac et al. (2008ApJ...681..187B), as well as by incorporating newly available data from the Cluster Lensing And Supernova survey with Hubble, we identified four systems of multiply lensed images (anew) in the redshift range 1.75<=z<=4.19. One multiple image system consists of in total eight multiply lensed images of the same source. The analysis based on a parametric mass model derived with the software GLAFIC suggests that the high image multiplicity is due to the source (z_phot_=4.19) being located on a so-called 'swallowtail' caustic. In addition to the parametric mass model, we also employed a non-parametric approach using the software pixelens in order to reconstruct the projected mass of the cluster using the same strong lensing data input. Both reconstructed mass models agree in revealing several mass components and a highly elliptic shape of the mass distribution. Furthermore, the projected mass inside, for example, a radius R~35arcsec~200kpc of the cluster for a source at redshift z=1.75 is M(<R)~(2.19^+0.01^_-0.02_)*10^14^M_{sun}_ as estimated by GLAFIC. Within the same radius pixelens predicts a mass of M(<R)~(2.47+/-0.01)*10^14^M_{sun}_which exceeds the GLAFIC estimate by ~13 per cent. The difference could be related to the fundamental degeneracy involved when constraining dark matter substructures with gravitationally lensed arcs.
- 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/A+AS/120/489
- Title:
- Galaxies morphology and IR photometry I.
- Short Name:
- J/A+AS/120/489
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Near Infrared (H-band) surface photometry of 158 (mostly) disk galaxies belonging to the Coma Supercluster and to the A262 and Cancer clusters was obtained using the 256^2^ NICMOS3 array MAGIC attached to the 2.2m Calar Alto telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices and total H magnitudes are derived.
- ID:
- ivo://CDS.VizieR/J/A+AS/120/521
- Title:
- Galaxies morphology and IR photometry II.
- Short Name:
- J/A+AS/120/521
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present near-infrared H-band (1.65{mu}m) surface photometry of 297 galaxies (mostly) in the Coma Supercluster obtained with the Arcetri NICMOS3 camera, ARNICA, mounted on the Gornergrat Infrared Telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices, and total H magnitudes are derived. Combining these observations with those obtained similarly using the Calar Alto telescopes (Paper I, <J/A+AS/120/489>) we find a strong positive correlation between the near-infrared concentration index and the galaxy H-band luminosity, and we analyze the consequent dependence of near-infrared growth-curves on H-band luminosity. For a description of the H band photometric system, see e.g. <GCPD/59>
- ID:
- ivo://CDS.VizieR/J/A+AS/142/65
- Title:
- Galaxies morphology and IR photometry III.
- Short Name:
- J/A+AS/142/65
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present near-infrared H-band (1.65{mu}m) surface photometry of 558 galaxies in the Coma Supercluster and in the Virgo cluster. This data set, obtained with the Arcetri NICMOS3 camera ARNICA mounted on the Gornergrat Infrared Telescope, is aimed at complementing, with observations of mostly early-type objects, our NIR survey of spiral galaxies in these regions, presented in previous papers of this series. Magnitudes at the optical radius, total magnitudes, isophotal radii and light concentration indices are derived. We confirm the existence of a positive correlation between the near-infrared concentration index and the galaxy H-band luminosity
- ID:
- ivo://CDS.VizieR/J/A+AS/142/73
- Title:
- Galaxies morphology and IR photometry IV.
- Short Name:
- J/A+AS/142/73
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present near-infrared (H band) surface photometry of 170 galaxies, obtained in 1997 using the Calar Alto 2.2 m telescope equipped with the NICMOS3 camera MAGIC. The majority of our targets are selected among bright members of the Virgo cluster, however galaxies in the A262 and Cancer clusters and in the Coma/A1367 supercluster are also included. This data set is aimed at complementing the NIR survey in the Virgo cluster discussed in Boselli et al. (1997A&A...324L..13B) and in the Coma Supercluster, presented in Papers I, II and III of this series. Magnitudes at the optical radius, total magnitudes, isophotal radii and light concentration indices are derived.
- ID:
- ivo://CDS.VizieR/J/A+A/361/863
- Title:
- Galaxies morphology and IR photometry. V.
- Short Name:
- J/A+A/361/863
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present near-infrared H-band (1.65{mu}m) surface brightness profile decomposition for 1157 galaxies in five nearby clusters of galaxies: Coma, A1367, Virgo, A262 and Cancer, and in the bridge between Coma and A1367 in the "Great Wall". The optically selected (m_pg_<=16.0) sample is representative of all Hubble types, from E to Irr+BCD, except dE and of significantly different environments, spanning from isolated regions to rich clusters of galaxies. We model the surface brightness profiles with a de Vaucouleurs r^1/4^ law (dV), with an exponential disk law (E), or with a combination of the two (B+D). From the fitted quantities we derive the H band effective surface brightness ({mu}_e_) and radius (r_e_) of each component, the asymptotic magnitude H_T_ and the light concentration index C_31_. We find that: i) Less than 50% of the Elliptical galaxies have pure dV profiles. The majority of E to Sb galaxies is best represented by a B+D profile. All Scd to BCD galaxies have pure exponential profiles. ii) The type of decomposition is a strong function of the total H band luminosity (mass), independent of the Hubble classification: the fraction of pure exponential decompositions decreases with increasing luminosity, that of B+D increases with luminosity. Pure dV profiles are absent in the low luminosity range L_H_<10^10^L_{sun}_ and become dominant above 10^11^L_{sun}_.
- ID:
- ivo://CDS.VizieR/J/MNRAS/332/422
- Title:
- Galaxies morphology and IR photometry. VIII
- Short Name:
- J/MNRAS/332/422
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the distribution of a statistical sample of nearby galaxies in the {kappa}-space ({kappa1}{prop.to}logM, {kappa}2{prop.to}log(Ie)^3^*M/L, {kappa}3{prop.to}M/L). Our study is based on near-IR (H-band: {lamdba}=1.65{mu}m) observations, for the first time comprising early- and late-type systems. Our data confirm that the mean effective dynamical mass-to-light ratio M/L of the E+S0+S0a galaxies increases with increasing effective dynamical mass M, as expected from the existence of the Fundamental Plane relation. Conversely, spiral and Im/BCD galaxies show broad distribution in M/L with no detected trend of M/L with M, the former galaxies having M/L values about twice larger than the latter, on average. For all the late-type galaxies, the M/L increases with decreasing effective surface intensity Ie, consistent with the existence of the Tully-Fisher relation.
- ID:
- ivo://CDS.VizieR/J/A+A/573/A93
- Title:
- Galaxies optical emission-line diagnostic diagrams
- Short Name:
- J/A+A/573/A93
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The discovery of the M-{sigma} relation, the local galaxy bimodality, and the link between black-hole and host-galaxy properties have raised the question of whether active galactic nuclei (AGN) play a role in galaxy evolution. AGN feedback is one of the biggest observational challenges of modern extragalactic astrophysics. Several theoretical models implement AGN feedback to explain the observed galaxy luminosity function and, possibly, the color and morphological transformation of spiral galaxies into passive ellipticals. For understanding the importance of AGN feedback, a study of the AGN populations in the radio-optical domain is crucial. A mass sequence linking star-forming galaxies and AGN has already been noted in previous works, and it is now investigated as a possible evolutionary sequence. We observed a sample of 119 intermediate-redshift (0.04<=z<0.4) SDSS-FIRST radio emitters with the Effelsberg 100-m telescope at 4.85 and 10.45GHz and obtained spectral indices. The sample includes star-forming galaxies, composite galaxies (with mixed contribution to line emission from star formation and AGN activity), Seyferts, and low ionization narrow emission region (LINER) galaxies. With these sources we search for possible evidence of spectral evolution and a link between optical and radio emission in intermediate-redshift galaxies. We find indications of spectral index flattening in high-metallicity star-forming galaxies, composite galaxies, and Seyferts. This "flattening sequence" along the [NII]-based emission-line diagnostic diagram is consistent with the hardening of galaxy ionizing field, thanks to nuclear activity. After combining our data with FIRST measurements at 1.4GHz, we find that the three-point radio spectra of Seyferts and LINERs show substantial differences, which are attributable to small radio core components and larger (arcsecond sized) jet/lobe components, respectively. A visual inspection of FIRST images seems to confirm this hypothesis. Galaxies along this sequence are hypothesized to be transitioning from the active star-forming galaxies (blue cloud) to the passive elliptical galaxies (red sequence). This supports the suggestion that AGN both play a role in shutting down star formation and allow the transition from one galaxy class to the other.
