We present a new catalog of galaxies in the wider region of the Virgo cluster, based on the Sloan Digital Sky Survey (SDSS) Data Release 7. The Extended Virgo Cluster Catalog (EVCC) covers an area of 725 deg 2 or 60.1 Mpc 2 . It is 5.2 times larger than the footprint of the classical Virgo Cluster Catalog (VCC) and reaches out to 3.5 times the virial radius of the Virgo cluster. We selected 1324 spectroscopically targeted galaxies with radial velocities less than 3000 km s −1 . In addition, 265 galaxies that have been missed in the SDSS spectroscopic survey but have available redshifts in the NASA Extragalactic Database are also included. Our selection process secured a total of 1589 galaxies of which 676 galaxies are not included in the VCC. The certain and possible cluster members are defined by means of redshift comparison with a cluster infall model. We employed two independent and complementary galaxy classification schemes: the traditional morphological classification based on the visual inspection of optical images and a characterization of galaxies from their spectroscopic features. SDSS u, g, r, i, and z passband photometry of all EVCC galaxies was performed using Source Extractor. We compare the EVCC galaxies with the VCC in terms of morphology, spatial distribution, and luminosity function. The EVCC defines a comprehensive galaxy sample covering a wider range in galaxy density that is significantly different from the inner region of the Virgo cluster. It will be the foundation for forthcoming galaxy evolution studies in the extended Virgo cluster region, complementing ongoing and planned Virgo cluster surveys at various wavelengths.Subject headings: catalogs -surveys -galaxies: clusters: general the spectroscopic data for refined classification of galaxies in the Virgo cluster region.We organize this paper as follows. Section 2 describes the definition of the EVCC region and the selection of galaxies. In section 3, we introduce two schemes of galaxy classification based on the SDSS imaging and spectroscopic data. Galaxy photometry is described in section 4 and the final EVCC catalog is presented in section 5. In section 6, we present a comparison between the EVCC and VCC. Finally, we summarize our results in section 7. SELECTION OF GALAXIES DataThe construction of the EVCC is based on the SDSS Data Release 7 (DR7) (Abazajian et al. 2009). The SDSS DR7 provides reduced and calibrated images taken in the u, g, r, i, and z bands with an effective exposure time of 54s in each band (see also Stoughton et al. 2002). The pixel scale of 0.396 arcsec and the average seeing of 1.4 arcsec correspond to a physical size of 32 pc and 112 pc, respectively, at a Virgo cluster distance of 16.5 Mpc (i.e., a distance modulus m − M = 31.1; Jerjen et al. 2004;Mei et al. 2007). The SDSS spectroscopic survey covers nominally all galaxies brighter than r ≤ 17.77 and r-band Petrosian half-light surface brightnesses µ 50 ≤ 24.5 mag arcsec −2 (Strauss et al. 2002). It provides fiber spectra with a wavelength coverage between 380...

In our recent report, observational evidence supports that the rotational direction of a galaxy tends to be coherent with the average motion of its nearby neighbors within 1 Mpc. We extend the investigation to neighbors at farther distances, in order to examine if such dynamical coherence is found even in large scales. The Calar Alto Legacy Integral Field Area (CALIFA) survey data and the NASA-Sloan Atlas (NSA) catalog are used. From the composite map of velocity distribution of 'neighbor' galaxies within 15 Mpc from the CALIFA galaxies, the composite radial profiles of the luminosity-weighted mean velocity of neighbors are derived. These profiles show unexpectedly strong evidence of the dynamical coherence between the rotation of the CALIFA galaxies and the average line-of-sight motion of their neighbors within several Mpc distances. Such a signal is particularly strong when the neighbors are limited to red ones: the luminosity-weighted mean velocity at 1 < D ≤ 6 Mpc is as large as 30.6 ± 10.9 km s −1 (2.8σ significance to random spin-axis uncertainty) for central rotation (R ≤ R e ). In the comparison of several subsamples, the dynamical coherence tends to be marginally stronger for the diffuse or kinematically-well-aligned CALIFA galaxies. For this mysterious coherence in large scales, we cautiously suggest a scenario that it results from a possible relationship between the long-term motion of a large-scale structure and the rotations of galaxies in it.

We present BV I surface photometry of 31 dwarf galaxy candidates discovered in a deep image stack from the KMTNet Supernova Program of ∼ 30 square degrees centered on the nearby NGC 2784 galaxy group. Our final images have a 3σ surface brightness detection limit of µ V ≈ 28.5 mag arcsec −2 . The faintest central surface brightness that we measure is µ 0,V = 26.1 mag arcsec −2 . If these candidates are at the distance of NGC 2784, then they have absolute magnitudes greater than M V = −9.5 mag and effective radii larger than 170 pc. Their radial number density decreases exponentially with distance from the center of NGC 2784 until it flattens beyond a radius of 0.5 Mpc. We interpret the baseline density level to represent the background contamination and so estimate that 22 of the 31 new candidates are dwarf members of the group. The candidate's average color, (B − V ) 0 ≈ 0.7, and Sérsic structural parameters are consistent with those parameters for the dwarf populations of other groups. We find that the central population of dwarfs is redder and brighter than the rest of the population. The measured faint end slope of the luminosity function, α ≈ −1.33, is steeper than that of the Local Group but consistent with published results for other groups. Such comparisons are complicated by systematic differences among different studies, but will be simpler when the KMTNet survey, which will provide homogenous data for 15 to 20 groups, is completed.