Семинар 96 – 5 апреля 2018 г.


Доклад: Как мы искали толстые диски в основной плоскости edge-on галактик

Иван Катков

По мотивам статьи "Imprint of the thick stellar disc in the mid-plane of edge-on galaxies", готовящейся к отправке в журнал.

Презентация

Анатолий Засов

1804.00469 TRGB distances to galaxies in front of the Virgo cluster

Igor D. Karachentsev, Lidia N. Makarova, R. Brent Tully, Luca Rizzi, Edward J. Shaya

Published 2018-04-02, 24 pages, 5 figures, 3 tables, accepted to ApJ

Tip of the red giant branch distances are acquired from Hubble SpaceTelescope images for 16 galaxies to the foreground of the Virgo Cluster. Thenew distances with 5% accuracy, combined with archival measurements, tightlyconstrain the near side location of the onset of infall into the Virgo Clusterto be 7.3+-0.3 Mpc from the cluster, reaching within 9 Mpc of the Milky Way.The mass within this turnaround radius about the cluster is 8.3+-0.9 x 10^{14}Msun. Color-magnitude diagrams are provided for galaxies in the study and thereis brief discussion of their group affiliations.

1803.09768 Dark Matter in Ultra-Diffuse Galaxies in the Virgo Cluster from their Globular Cluster Populations

Elisa Toloba, Sungsoon Lim, Eric Peng, Laura V. Sales, Puragra Guhathakurta, J. Christopher Mihos, Patrick Cote, Alessandro Boselli, Jean-Charles Cuillandre, Laura Ferrarese, Stephen Gwyn, Ariane Lancon, Roberto Munoz, Thomas Puzia

Published 2018-03-26, 8 pages, 5 figures. Accepted for publication in The Astrophysical Journal Letters

We present Keck/DEIMOS spectroscopy of globular clusters (GCs) around theultra-diffuse galaxies (UDGs) VLSB-B, VLSB-D, and VCC615 located in the centralregions of the Virgo cluster. We spectroscopically identify 4, 12, and 7 GCsatellites of these UDGs, respectively. We find that the three UDGs havesystemic velocities ($V_{sys}$) consistent with being in the Virgo cluster, andthat they span a wide range of velocity dispersions, from $\sim 16$ to $\sim47$ km/s, and high dynamical mass-to-light ratios within the radius thatcontains half the number of GCs ($ 407^{+916}_{-407}$, $21^{+15}_{-11}$,$60^{+65}_{-38}$, respectively). VLSB-D shows possible evidence for rotationalong the stellar major axis and its $V_{sys}$ is consistent with that of themassive galaxy M84 and the center of the Virgo cluster itself. These findings,in addition to having a dynamically and spatially ($\sim 1$ kpc) off-centerednucleus and being extremely elongated, suggest that VLSB-D could be tidallyperturbed. On the contrary, VLSB-B and VCC615 show no signals of tidaldeformation. Whereas the dynamics of VLSB-D suggest that it has a less massivedark matter halo than expected for its stellar mass, VLSB-B and VCC615 areconsistent with a $\sim 10^{12}$ M$_{\odot}$ dark matter halo. Although oursamples of galaxies and GCs are small, these results suggest that UDGs may be adiverse population, with their low surface brightnesses being the result ofvery early formation, tidal disruption, or a combination of the two.