2012A&A...538A..87S


Query : 2012A&A...538A..87S

2012A&A...538A..87S - Astronomy and Astrophysics, volume 538A87-87 (2012/2-1)

Kinematic properties of the field elliptical NGC 7507.

SALINAS R., RICHTLER T., BASSINO L.P., ROMANOWSKY A.J. and SCHUBERTH Y.

Abstract (from CDS):

The dark matter (DM) halos of field elliptical galaxies have not been well-studied and their properties appear controversial in the literature. While some galaxies appear to be nearly devoid of DM, others show clear evidence of its presence. Furthermore, modified Newtonian dynamics (MOND), which has been found to have predictive power in the domain of disk galaxies, has not yet been investigated for isolated elliptical galaxies. We study the kinematics of the isolated elliptical NGC 7507, which has been claimed as a clear example of DM presence in early-type galaxies. We obtained major and minor axis long-slit spectroscopy of NGC 7507 using the Gemini South telescope and deep imaging in Kron-Cousins R and Washington C using the CTIO/MOSAIC camera. Mean velocities, velocity dispersion and higher order moments of the velocity distribution are measured out to ∼90''. The galaxy, although almost circular, has significant rotation along the minor axis and a rapidly declining velocity dispersion along both axes. The velocity dispersion profile is modeled in the context of a spherical Jeans analysis. Models without DM provide an excellent representation of the data with a mass-to-light ratio (M/L) of 3.1 (R-band). The most massive Navarro-Frenk-White (NFW) halo the data allow has a virial mass of only 3.9+3.1–2.1x1011M☉, although the data are more consistent with models that have a slight radial anisotropy, which implies the galaxy has an even lower DM halo mass of 2.2+2.0–1.2x1011M☉. Modeling of the h4 Gauss-Hermite coefficient is inconclusive but seems to be consistent with mild radial anisotropy. A cored logarithmic DM halo with parameters r0=7kpc and v0=100km/s can also reproduce the observed velocity dispersion profile. The MOND predictions overestimate the velocity dispersion. In conclusion, we cannot easily reproduce the previous findings of a predominance of DM in NGC 7507 within a simple spherical model. DM may be present, but only in conjunction with a strong radial anisotropy, for which there are some indications.

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Journal keyword(s): galaxies: individual: NGC 7507 - Galaxy: kinematics and dynamics

Simbad objects: 13

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Number of rows : 13
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 NGC 821 AG? 02 08 21.1358498040 +10 59 41.832436704   12.210 11.310 10.739 9.744 ~ 592 0
2 NGC 1399 rG 03 38 29.083 -35 27 02.67 11.05 9.74 9.59 8.12   ~ 1636 1
3 NGC 1400 EmG 03 39 30.851 -18 41 17.25 12.48 12.01 10.96 10.45   ~ 309 1
4 NGC 3311 EmG 10 36 42.821 -27 31 42.02   11.93 10.93 10.00 9.67 ~ 310 2
5 M 105 LIN 10 47 49.600 +12 34 53.87   10.56 9.76 9.12 8.18 ~ 1504 0
6 M 84 Sy2 12 25 03.74333 +12 53 13.1393 12.67 12.09 10.49     ~ 1841 2
7 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7815 3
8 NGC 4494 GiP 12 31 24.0391348536 +25 46 30.071664120   10.55 9.74     ~ 491 0
9 NGC 4636 LIN 12 42 49.8333280080 +02 41 15.951929028   12.62 11.84     ~ 1156 1
10 NGC 4697 GiG 12 48 35.8981498824 -05 48 02.482374564   10.97   9.83   ~ 895 0
11 NGC 6166 Sy2 16 28 38.24470063 +39 33 04.2335319   12.78 11.78     ~ 793 2
12 NGC 7507 GiG 23 12 07.595 -28 32 22.70   11.60   9.98   ~ 184 0
13 NGC 7513 EmG 23 13 14.0669738568 -28 21 27.280137168   12.73   11.40   ~ 94 0

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