2019ApJ...885..153B

Query : 2019ApJ...885..153B

2019ApJ...885..153B - Astrophys. J., 885, 153-153 (2019/November-2)

The M101 satellite luminosity function and the halo-halo scatter among Local Volume hosts.

BENNET P., SAND D.J., CRNOJEVIC D., SPEKKENS K., KARUNAKARAN A., ZARITSKY D. and MUTLU-PAKDIL B.

Abstract (from CDS):

We have obtained deep Hubble Space Telescope (HST) imaging of 19 dwarf galaxy candidates in the vicinity of M101. Advanced Camera for Surveys HST photometry for two of these objects showed resolved stellar populations and tip of the red giant branch derived distances (D ∼ 7 Mpc) consistent with M101 group membership. The remaining 17 were found to have no resolved stellar populations, meaning they are either part of the background NGC 5485 group or are distant low surface brightness (LSB) galaxies. It is noteworthy that many LSB objects that had previously been assumed to be M101 group members based on projection have been shown to be background objects, indicating the need for future diffuse dwarf surveys to be very careful in drawing conclusions about group membership without robust distance estimates. In this work we update the satellite luminosity function of M101 based on the presence of these new objects down to MV = -8.2. M101 is a sparsely populated system with only nine satellites down to MV ≃ -8, as compared with 26 for M31 and 24.5 ± 7.7 for the median host in the Local Volume. This makes M101 by far the sparsest group probed to this depth, although M94 is even sparser to the depth at which it has been examined (MV = -9.1). M101 and M94 share several properties that mark them as unusual compared with the other Local Volume galaxies examined: they have a very sparse satellite population but also have high star-forming fractions among these satellites; such properties are also found in the galaxies examined as part of the Satellites around Galactic Analogs survey. We suggest that these properties appear to be tied to the wider galactic environment, with more isolated galaxies showing sparse satellite populations that are more likely to have had recent star formation, while those in dense environments have more satellites that tend to have no ongoing star formation. Overall, our results show a level of halo-to-halo scatter between galaxies of similar mass that is larger than is predicted in the lambda cold dark matter model.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

Journal keyword(s): Dwarf galaxies - Luminosity function - Galaxy evolution - HST photometry - Galaxy stellar halos - Galaxy groups

Simbad objects: 51

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Number of rows : 51
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 M 31 AGN 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 13622 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 7988 0
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 19090 0
4 NAME M 81-82 Group GrG 09 55 +69.1           ~ 758 0
5 M 81 Sy2 09 55 33.1726556496 +69 03 55.062505368   7.89 6.94     ~ 4725 3
6 M 82 AGN 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 6156 6
7 NGC 3077 GiP 10 03 19.0965510921 +68 44 01.556166166 11.23 10.85 10.14 9.74   ~ 808 0
8 NAME Virgo Cluster ClG 12 30 47.8 +12 23 07           ~ 7107 0
9 M 94 SyG 12 50 53.0737971432 +41 07 12.900884628 9.15 8.96 8.24 7.78   ~ 1476 2
10 ACO 1656 ClG 12 59 44.40 +27 54 44.9           ~ 5141 2
11 NAME Cen A Group GrG 13 20 33.9 -44 58 51           ~ 274 0
12 NAME Centaurus A BLL 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4774 3
13 [CSC2014] CenA-MM-Dw2 G 13 29 57.34 -41 52 22.6           ~ 14 0
14 Z 272-13 AG? 13 54 45.602 +53 54 20.06   14.2       ~ 219 0
15 [BSC2017] Dw 9 LSB 13 55 44.6 +55 08 45           ~ 11 0
16 MCG+09-23-020 LSB 13 57 14.6983598016 +54 06 03.171260340   16.0       ~ 28 0
17 MATLAS-1691 LSB 14 01 40.3 +55 00 57           ~ 5 0
18 MATLAS-1692 LSB 14 02 20.0 +55 39 19           ~ 6 0
19 NAME M101 Group GrG 14 03 +54.3           ~ 112 1
20 [MVA2014] DF 3 LSB 14 03 05.7 +53 36 56   17.9       ~ 21 0
21 M 101 GiP 14 03 12.583 +54 20 55.50   8.46 7.86 7.76   ~ 3138 2
22 SMDG J1403450+535638 LSB 14 03 45.0 +53 56 40   18.9       ~ 21 0
23 MATLAS-1703 LSB 14 04 13.0 +55 43 35           ~ 4 0
24 [KRZ2015] M 101 dwD LSB 14 04 24.6 +53 16 19   19.2       ~ 7 0
25 MATLAS-1704 LSB 14 04 24.8 +55 06 14           ~ 6 0
26 [MVA2014] DF 5 LSB 14 04 28.1 +55 37 00           ~ 9 0
27 NGC 5473 GiG 14 04 43.2276404712 +54 53 33.499699368   12.5       ~ 156 0
28 NGC 5474 GiP 14 05 01.608 +53 39 43.95   11.28 10.79     ~ 475 1
29 MATLAS-1708 LSB 14 05 18.1 +54 53 52   20.2       ~ 9 0
30 NGC 5477 AG? 14 05 33.318 +54 27 37.85 13.94 14.36 14.01     ~ 224 1
31 [MVA2014] DF 7 LSB 14 05 47.50 +55 07 57.3   20.4       ~ 13 0
32 SMDG J1406499+534430 LSB 14 06 49.9 +53 44 30   19.2       ~ 17 0
33 NGC 5485 LIN 14 07 11.3594809920 +55 00 06.084219996 14.34 13.82 12.22     ~ 267 0
34 MATLAS-1730 LSB 14 07 21.0 +55 03 51           ~ 7 0
35 [MVA2014] DF 4 LSB 14 07 33.80 +54 42 39.2   18.8       ~ 14 0
36 [BSC2017] Dw 13 LSB 14 08 01.2 +54 22 30           ~ 3 0
37 [MVA2014] DF 6 LSB 14 08 18.70 +55 11 30.6   20.1       ~ 11 0
38 SMDG J1408374+541932 LSB 14 08 37.5 +54 19 31   19.8       ~ 20 0
39 MATLAS-1754 LSB 14 08 43.7 +55 10 02   20.1       ~ 9 0
40 MATLAS-1755 LSB 14 08 45.8 +55 17 13           ~ 6 0
41 [BSC2017] Dw 15 LSB 14 09 17.5 +53 45 30           ~ 3 0
42 MATLAS-1765 LSB 14 09 21.9 +55 18 15           ~ 3 0
43 [BSC2017] Dw 12 LSB 14 09 26.0 +54 14 51           ~ 2 0
44 [BSC2017] Dw 11 LSB 14 10 04.8 +54 15 29           ~ 4 0
45 SMDG J1410597+555328 LSB 14 10 59.7 +55 53 29           ~ 4 0
46 [BSC2017] Dw 14 LSB 14 11 03.2 +53 56 50           ~ 4 0
47 SMDG J1413016+551117 LSB 14 13 01.7 +55 11 16           ~ 5 0
48 LEDA 50911 G 14 15 08.593 +57 05 30.99   16.5       ~ 35 0
49 MCG+10-21-013 AG? 14 35 24.077 +57 15 21.24   17       ~ 91 0
50 NGC 6181 H2G 16 32 20.96927 +19 49 35.7710   12.7       ~ 258 1
51 NAME Local Group GrG ~ ~           ~ 9325 0

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