The SLUGGS Survey: new evidence for a tidal interaction between the early-type galaxies NGC 4365 and NGC 4342

Blom, Christina; Forbes, Duncan A.; Foster, Caroline; Romanowsky, Aaron J.; Brodie, Jean P.

doi:10.1093/mnras/stu095

Cited by 51 publications

(48 citation statements)

References 65 publications

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“…A number of companion galaxies are projected on or near the tail, most notably the S0 galaxy NGC 4342 (761 km s −1 , Cappellari et al 2011). While Bogdán et al argued the tail was unlikely to have been stripped from NGC 4342, due to the high dark halo mass implied by the galaxy's Xray luminosity, subsequent observations by Blom et al (2012aBlom et al ( , 2014 of globular clusters in the stream showed a convincing kinematic match between the tidal tail and NGC 4342. Figure 9b shows a deep stretch of our B band image, after masking of bright sources.…”

Section: The M49 Fieldmentioning

confidence: 97%

The Burrell Schmidt Deep Virgo Survey: Tidal Debris, Galaxy Halos, and Diffuse Intracluster Light in the Virgo Cluster

Mihos

Harding

Feldmeier

et al. 2016

ApJ

164

154

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We present the results of a deep imaging survey of the Virgo cluster of galaxies, concentrated around the cores of Virgo subclusters A and B. The goal of this survey was to detect and study very low surface brightness features present in Virgo, including discrete tidal features, the faint halos of luminous galaxies, and the diffuse intracluster light (ICL). Our observations span roughly 16 degrees 2 in two filters, reaching a 3σ limiting depth of µ B =29.5 and µ V =28.5 mag arcsec −2 . At these depths, our limiting systematic uncertainties are astrophysical: variations in faint background sources as well as scattered light from galactic dust. We show that this dust-scattered light is well-traced by deep farinfrared imaging, making it possible to separate it from true diffuse light in Virgo. We use our imaging to trace and measure the color of the diffuse tidal streams and intracluster light in the Virgo core near M87, in fields adjacent to the core including the M86/M84 region, and to the south of the core around M49 and subcluster B, along with the more distant W cloud around NGC 4365. Overall, the bulk of the projected ICL is found in the Virgo core and within the W cloud; we find little evidence for an extensive ICL component in the field around M49. The bulk of the ICL we detect is fairly red in color (B − V =0.7-0.9), indicative of old, evolved stellar populations. Based on the luminosity of the observed ICL features in the cluster, we estimate a total Virgo ICL fraction of 7-15%. This value is somewhat smaller than that expected for massive, evolved clusters, suggesting that Virgo is still in the process of growing its extended ICL component. We also trace the shape of M87's extremely boxy outer halo out to ∼ 150 kpc, and show that the current tidal stripping rate from low luminosity galaxies is insufficient to have built M87's outer halo over a Hubble time. We identify a number of previously unknown low surface brightness structures around galaxies projected close to M86 and M84. The extensive diffuse light seen in the infalling W cloud around NGC 4365 is likely to be subsumed in the general Virgo ICL component once the group enters the cluster, illustrating the importance of group infall in generating intracluster light. Finally, we also identify another large and extremely low surface brightness ultra-diffuse galaxy, likely in the process of being shredded by the cluster tidal field. With the survey complete, the full imaging dataset is now available for public release.

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Section: The M49 Fieldmentioning

confidence: 97%

The Burrell Schmidt Deep Virgo Survey: Tidal Debris, Galaxy Halos, and Diffuse Intracluster Light in the Virgo Cluster

Mihos

Harding

Feldmeier

et al. 2016

ApJ

164

154

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“…We note that there are uncertainties associated with the bulge luminosity for NGC 1332 (see Kormendy & Ho 2013 for details) and the black hole mass measurement for NGC 4486B (see Gültekin et al 2009 for details). Also, tidal stripping is believed to be the cause of the over-massive black hole in the ultracompact dwarf galaxy M60-UCD1 (Seth et al 2014), and there is some debate as to whether NGC 4486B and NGC 4342 have been stripped as well (e.g., Faber., 1973;Bogdán et al 2012;Blom et al 2014). Nevertheless, additional similar galaxies need to be studied because there could be systematic differences in the scaling relations between the compact, high-dispersion galaxies and the giant ellipticals/BCGs.…”

Section: Introductionmentioning

confidence: 99%

The Black Hole in the Compact, High-Dispersion Galaxy NGC 1271

Walsh

Bosch

Gebhardt

et al. 2015

ApJ

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Located in the Perseus cluster, NGC 1271 is an early-type galaxy with a small effective radius of 2.2 kpc and a large bulge stellar velocity dispersion of 276 km s −1 for its K-band luminosity of L 8.9 10 10  . We present a mass measurement for the black hole in this compact, high-dispersion galaxy using observations from the Near-infrared Integral Field Spectrometer on the Gemini North telescope assisted by laser guide star adaptive optics, large-scale integral field unit observations with PPAK at the Calar Alto Observatory, and Hubble Space Telescope WFC3 imaging observations. We are able to map out the stellar kinematics both on small spatial scales, within the black hole sphere of influence, and on large scales that extend out to four times the galaxy's effective radius. We find that the galaxy is rapidly rotating and exhibits a sharp rise in the velocity dispersion. Through the use of orbit-based stellar dynamical models, we determine that the black hole has a mass of M (3.0 ) 10 1.1 1.0 9 -+  and the H-band stellar mass-to-light ratio is 1.40 0.11 0.13 ¡ -+  (1s uncertainties). NGC 1271 occupies the sparsely populated upper end of the black hole mass distributionbut is very different from the brightest cluster galaxies (BCGs) and giant elliptical galaxies that are expected to host the most massive black holes. Interestingly, the black hole mass is an order of magnitude larger than expectations based on the galaxy's bulge luminositybut is consistent with the mass predicted using the galaxy's bulge stellar velocity dispersion. More compact, high-dispersion galaxies need to be studied using high spatial resolution observations to securely determine black hole masses, as there could be systematic differences in the black hole scaling relations between these types of galaxies and the BCGs/giant ellipticals, thereby implying different pathways for black hole and galaxy growth.

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“…Coccato et al 2009;Usher et al 2012;Pota et al 2013), but so far has had very limited application to visible substructures. Pioneering examples include PN-and GC-based spectroscopic studies of tidal debris around M51 (Durrell et al 2003), of an outer halo stream in M87 (Romanowsky et al 2012), of substructures around M31 (Veljanoski et al 2013), and of a tidal stream linking NGC 4365 and NGC 4342 (Blom et al 2014). …”

Section: Introductionmentioning

confidence: 99%

Kinematics and simulations of the stellar stream in the halo of the Umbrella Galaxy

Foster

Lux

Romanowsky

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We study the dynamics of faint stellar substructures around the Umbrella Galaxy, NGC 4651, which hosts a dramatic system of streams and shells formed through the tidal disruption of a nucleated dwarf elliptical galaxy. We elucidate the basic characteristics of the system (colours, luminosities, stellar masses) using multi-band Subaru/Suprime-Cam images. The implied stellar mass-ratio of the ongoing merger event is ∼ 1:50. We identify candidate kinematic tracers (globular clusters, planetary nebulae, H ii regions), and follow up a subset with Keck/DEIMOS spectroscopy to obtain velocities. We find 15 of the tracers are likely associated with halo substructures, including the probable stream progenitor nucleus. These objects delineate a kinematically cold feature in position-velocity phase space. We model the stream using single test-particle orbits, plus a rescaled pre-existing N-body simulation. We infer a very eccentric orbit with a period of ∼ 0.35 Gyr and turning points at ∼ 2-4 and ∼ 40 kpc, implying a recent passage of the satellite through the disc, which may have provoked the visible disturbances in the host galaxy. This work confirms that the kinematics of low surface brightness substructures can be recovered and modelled using discrete tracers -a breakthrough that opens up a fresh avenue for unraveling the detailed physics of minor merging.

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The SLUGGS Survey: new evidence for a tidal interaction between the early-type galaxies NGC 4365 and NGC 4342

Cited by 51 publications

References 65 publications

The Burrell Schmidt Deep Virgo Survey: Tidal Debris, Galaxy Halos, and Diffuse Intracluster Light in the Virgo Cluster

The Burrell Schmidt Deep Virgo Survey: Tidal Debris, Galaxy Halos, and Diffuse Intracluster Light in the Virgo Cluster

The Black Hole in the Compact, High-Dispersion Galaxy NGC 1271

Kinematics and simulations of the stellar stream in the halo of the Umbrella Galaxy

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