Stellar populations and kinematics of dwarf galaxies in the Virgo cluster with Gemini-GMOS

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1 Stellar populations and kinematics of dwarf galaxies in the Virgo cluster with Gemini-GMOS Richard McDermid Macquarie University / Australian Astronomical Observatory MACQUARIE University

2 Dwarfs Test Models: Number Density Weinmann+1! Number density of dwarfs evolves more strongly than predicted

3 Dwarfs Test Models: Star Formation Semi-Analytic Model Observations More Star Forming Weinmann+1 Salim+7 (SDSS)! ssfr increases at lower mass, opposite to predictions

4 Dwarfs are Sensitive to Environment Fraction of passive galaxies Cluster Number Density Field Log Mass zcosmos Peng+1

5 Dwarfs are Sensitive to Environment Geha & Blanton 1! For log(m)<9., there are no quenched galaxies

6 Dwarfs are Sensitive to Environment! For log(m)<9., there are no quenched galaxies! Extends to larger masses, but non-zero quenched fraction Geha & Blanton 1

7 Ram-Pressure Stripping of Dwarfs UV / Hα trail Away from cluster Smith+1! Asymmetric UV and Hα trails are seen in Coma dwarfs

8 Ram-Pressure Stripping of Dwarfs Smith+1! Asymmetric UV and Hα trails are seen in Coma dwarfs! Tails indicate mostly incoming events triggered on first traverse

9 Ram-Pressure Stripping of Dwarfs Smith+1! Asymmetric UV and Hα trails are seen in Coma dwarfs! Tails indicate mostly incoming events triggered on first traverse! Stripping is specific to cluster centre most aggressive region

10 Environment Impacting Dynamics Angular Momentum Late Types Early Types Toloba+14 Ellipticity! Dwarf early-types have lower angular momentum than spirals

11 Environment Impacting Dynamics Angular Momentum Toloba+14 Distance from Centre of Virgo! Suggestive dependence on distance from cluster centre

12

13 Targeting the Densest Dwarfs with GMOS Stripping Models

14 Targeting the Densest Dwarfs with GMOS Guerou, Emsellem, McDermid + NGVS, 15

15 Targeting the Densest Dwarfs with GMOS! Cover from Re/3 to >Re Guerou, Emsellem, McDermid + NGVS, 15

16 Targeting the Densest Dwarfs with GMOS Strong Disky Residuals! Cover from Re/3 to >Re! Half of sample shows disky residuals from ellipse fit

17 V (km/s) σ (km/s) Age (Gyr) [Z/H] 4 VCC3 - [arcsec] -4 / 4 / 1 5 / / VCC1178 VCC119-1 / 1-4 / 4 5 / 16 / 1 6 / 1 8 / / / [arcsec] [arcsec] -4 4 VCC / 35 / 6 7 / 13-8 / 8 1 / 5 9 / /.3 -. / [arcsec] 7

18 1 / 5 Age (Gyr) 9 / 11 - [Z/H] -. / / 4 / 1 5 / /-. -4 / 4 / 8 8 / /. [arcsec] VCC197 VCC / // [arcsec] 6 / 1 5 / // // 11-1 / 1 [arcsec] -3 // VCC144 VCC1178 VCC1475 VCC119 [arc -. /.3 σ (km/s) 7 / 13 V (km/s) / 6-35 / 35 VCC Gu erou et al. -8 / / 8 [arcsec] / 5 [arcsec] -. /.3 / 5 7 / 13-3 / 3 / 6 8 / / /.3 [arcsec] /.1 [arcsec] [arcsec] -35 / 35 VCC167 VCC

19 VCC1475: Counter-Rotating Disk V -(km/s) 3 σ -(km/s) 1 y [arcsec] V -(km/s) x [arcsec] GMOS/IFU Koleva x [arcsec] Fig. 6. Radial stellar velocity, V, and velocity dispersion, σ, mapsforvcc1475fromgmos-ifudata(toprow). Thexandyaxesare both in arcseconds. The black dotted lines indicate the region of the galaxy observed with a long-slit Guerou, by Koleva etemsellem, al. (11b). The bottom panels show comparisons of the Koleva et al. (11b) V and σ profiles with comparable long-slit data simulated from our GMOS-IFU observations. The error bars are computed using the light weighted standard deviation of the points considered within the simulated slit. Koleva et al. (11b) error bars are typically of.7 km s 1 and are smaller than the marker points.! Suggested by long-slit, confirmed by IFU later re-analyzed by Toloba et al. (14a). This galaxy is located in the outskirts of the cluster, about 1.1 Mpc in (long slit) σ -(km/s) McDermid + NGVS, 15 Like VCC 197, this σ galaxy has a stellar population that is 1 Gyr younger in its core region than in the

20 General Picture Zone of Avoidance Atlas3D - Cappellari et al. 13b

21 Massive Early-Types: Mass-Size Plane Age [Z/H] [α/fe] Locally-weighted average values Atlas3D: McDermid et al. (15)

22 Extending Mass and Environment Range Guerou, Emsellem, McDermid + NGVS, 15! Compact dwarfs age and metallicity follow same mass-size trend! Values comparable to massive early-types

23 Extending Mass and Environment Range R e [pc]! Guerou, Emsellem, McDermid + NGVS, 15! No obvious trend with number density

24 Extending Mass and Environment Range Guerou, Emsellem, McDermid + NGVS, 15! BUT: Strong trend with luminosity of brightest neighbour! Compact dwarfs dominated by bright companion

25 Trend with Dynamics?.6.5 GMOS-IFU Toloba+14b (λ Re /) Rys+14 (λ Re ) de(i), discy λr Guerou, Emsellem, McDermid + NGVS, ϵ! No obvious trend with angular momentum! Need larger samples to say much

26 Conclusions! Dwarf galaxies are sensitive probes of galaxy evolution! Test of star formation physics over long timescales! Test of environmental effects in dense regions! Stellar populations and kinematics of compact dwarfs similar to massive early-types! SAMI, MaNGA (+HECTOR) may help to boost samples! Faint, low velocity dispersion, and small apparent size: need large telescope+ifu for detailed studies

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