J/AJ/146/45 Spectroscopy of 6 early-type galaxies (Rusli+, 2013)
The influence of dark matter halos on dynamical estimates of black hole mass:
10 new measurements for high-σ early-type galaxies.
Rusli S.P., Thomas J., Saglia R.P., Fabricius M., Erwin P., Bender R.,
Nowak N., Lee C.H., Riffeser A., Sharp R.
<Astron. J., 146, 45 (2013)>
=2013AJ....146...45R 2013AJ....146...45R
ADC_Keywords: Galaxies, rotation ; Rotational velocities ; Velocity dispersion
Keywords: galaxies: elliptical and lenticular, cD -
galaxies: kinematics and dynamics - galaxies: nuclei
Abstract:
Adaptive optics assisted SINFONI observations of the central regions
of 10 early-type galaxies are presented. Based primarily on the
SINFONI kinematics, 10 black hole (BH) masses occupying the high-mass
regime of the MBH-σ relation are derived using three-integral
Schwarzschild models. The effect of dark matter (DM) inclusion on the
BH mass is explored. The omission of a DM halo in the model results in
a higher stellar mass-to-light ratio, especially when extensive
kinematic data are used in the model. However, when the diameter of
the sphere of influence--computed using the BH mass derived without a
dark halo--is at least 10 times the point-spread function FWHM during
the observations, it is safe to exclude a DM component in the
dynamical modeling, i.e., the change in BH mass is negligible. When
the spatial resolution is marginal, restricting the mass-to-light
ratio to the right value returns the correct MBH although a dark
halo is not present in the model. Compared to the MBH-σ and
MBH-L relations of McConnell et al., the 10 BHs are all more massive
than expected from the luminosities and 7 BH masses are higher than
expected from the stellar velocity dispersions of the host bulges.
Using new fitted relations, which include the 10 galaxies, we find
that the space density of the most massive BHs (MBH≳109M☉)
estimated from the MBH-L relation is higher than the estimate based
on the MBH-σ relation and the latter is higher than model
predictions based on quasar counts, each by about an order of
magnitude.
Description:
NGC1374 was observed during the period 2001 November 10-14 at the La
Silla ESO New Technology Telescope (NTT), equipped with the EMMI
spectrograph (wavelength range λ=8298-8893Å). NGC6861 was
observed during the period 2001 May 8-14 at the 2.3 Siding Spring
telescope, where we used the red arm of the double-beam spectrograph
(wavelength range λ=7645-9573Å).
The observations of NGC3091 and NGC5328 were carried out using the new
VIRUS-W spectrograph at the 2.7m Harlan J. Smith telescope at the
McDonald Observatory in Texas. NGC3091 was observed during the
commissioning of VIRUS-W in 2010 December, while for NGC5328 we were
granted with two nights of observing time in 2011 May. For both
galaxies, we used a resolution R=3300 and a spectral coverage of
4320-6042Å. We obtained dithered observations of two off-centered
and slightly overlapping regions of NGC3091 and NGC5328 on the night
of December 5 and the two nights of May 24 and 25, respectively.
NGC4751 and NGC5516 were observed in 2010 May at the ANU 2.3m
telescope at Siding Spring Observatory. The instrument was WiFeS (Wide
Field Spectrograph) Integral Field Spectrograph.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 68 10 The sample
table5.dat 59 9 The long-slit kinematics of NGC 1374
table6.dat 59 15 The long-slit kinematics of NGC 6861
table7.dat 62 100 The VIRUS-W kinematics of NGC 3091: four quadrants
table8.dat 62 25 The VIRUS-W kinematics of NGC 3091: the folded quadrant
table9.dat 69 46 The VIRUS-W kinematics of NGC 5328
table10.dat 64 108 The kinematics of NGC 4751 derived from WiFeS data
table11.dat 64 88 The kinematics of NGC 5516 derived from WiFeS data
table12.dat 69 54 The kinematics of NGC 4751: the folded quadrant
table13.dat 69 44 The kinematics of NGC 5516: the folded quadrant
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See also:
J/ApJ/754/67 : Longslit spectroscopy of local bulges (Fabricius+, 2012)
J/AJ/144/78 : Spectroscopy of early-type galaxies in A262 (Wegner+, 2012)
J/A+A/516/A4 : NGC1600, NGC4125, NGC7619 extended spectroscopy (Pu+, 2010)
J/A+AS/145/263 : Kinematical data on early-type galaxies. V. (Simien+, 2000)
J/A+A/296/319 : Fornax cluster early-type galaxies (D'Onofrio+, 1995)
J/A+AS/105/433 : Kinematical data of 14 early-type galaxies (Longo+ 1994)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [NGC]
5- 8 I4 --- NGC Galaxy NGC number
10- 13 A4 --- MType Galaxy type (E or E/S0) (1)
15- 19 F5.2 Mpc Dist Distance (2)
20 A1 --- f_Dist [*] Distance adopted from the SBF survey (3)
22- 27 F6.2 mag BMag Absolute B-band magnitude (4)
29- 34 F6.2 mag VMag Absolute V-band magnitude (5)
36- 40 F5.1 arcsec Reff Effective radius (6)
42- 46 F5.1 km/s sigma HyperLeda central velocity dispersion
48- 51 F4.1 km/s e_sigma Uncertainty in sigma
53- 57 F5.1 km/s sig(e) Velocity dispersion within Reff (see Section 8)
59- 62 F4.1 km/s e_sig(e) Uncertainty in sig(e)
64- 68 A5 --- Tables Tables with profile data
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Note (1): From HyperLeda (http://leda.univ-lyon1.fr) except for NGC5516, which
we classify as E based on our kinematics and photometry.
Note (2): Calculated from the radial velocity corrected for the infall velocity
of Local Group to the Virgo cluster (HyperLeda) assuming H0=72km/s except
for NGC4472 where we take the SBF distance from Mei et al.
(2007, cat. J/ApJ/655/144).
Note (3): Tonry et al. (2001ApJ...546..681T 2001ApJ...546..681T). After applying the Cepheid
zero-point correction of -0.06mag (Mei et al., 2005ApJ...625..121M 2005ApJ...625..121M).
Note (4): Taken from HyperLeda, used only to calculate the appropriate dark halo
parameters based on the scaling relation in Thomas et al.
(2009ApJ...691..770T 2009ApJ...691..770T)-see Equations (2) and (3).
Note (5): For all galaxies but NGC 4751 and NGC 5516, VMag is derived from the
B0T magnitude and B-V color index of RC3. For NGC4751, VMag is
calculated from a V magnitude of 11.80 from NED, and for NGC5516 VMag is
obtained from total B magnitude and B-V color index from HyperLeda. All
VMag values are corrected for the foreground Galactic extinction of
Schlegel et al. (1998ApJ...500..525S 1998ApJ...500..525S).
Note (6): From RC3 (except for NGC4472, where we use the value of Caon et al.,
1994, cat. J/A+AS/106/199).
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Byte-by-byte Description of file: table[56].dat
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Bytes Format Units Label Explanations
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1- 6 F6.2 arcsec R Position within the slit (G1)
8- 14 F7.2 km/s V(R) Stellar rotational velocity (relative to V(0))
16- 20 F5.2 km/s e_V(R) Uncertainty in V(R)
22- 27 F6.2 km/s sigma Stellar velocity dispersion σ
29- 33 F5.2 km/s e_sigma Uncertainty in sigma
35- 40 F6.3 --- h3 First order of asymmetric deviation (1)
42- 46 F5.3 --- e_h3 Uncertainty in h3
48- 53 F6.3 --- h4 First order of symmetric deviation (1)
55- 59 F5.3 --- e_h4 Uncertainty in h4
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Note (1): Of the line-of-sight velocity distribution (LOSVD) from real
Gaussian profile.
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Byte-by-byte Description of file: table[78].dat
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Bytes Format Units Label Explanations
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1- 6 F6.2 arcsec R [-42.29/42.29] Radial midpoint of each bin (1)
8- 9 I2 --- iv [-5/5] Numbering of the angular bin (1)
11- 17 F7.2 km/s V(R) Stellar rotational velocity (relative to average)
19- 23 F5.2 km/s e_V(R) Uncertainty in V(R)
25- 30 F6.2 km/s sigma Stellar velocity dispersion σ
32- 36 F5.2 km/s e_sigma Uncertainty in sigma
38- 43 F6.3 --- h3 Gauss-Hermite moment, h3
45- 49 F5.3 --- e_h3 Uncertainty in h3
51- 56 F6.3 --- h4 Gauss-Hermite moment, h4
58- 62 F5.3 --- e_h4 Uncertainty in h4
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Note (1): See Section 3. Every quadrant consists of five angular bins whose
centers are at the angles 5.8° (iv=1), 17.6° (iv=2), 30.2°
(iv=3), 45.0° (iv=4), and 71.6° (iv=5). The sign of the Rad and iv
indicate the quadrant in which the bin is located. Positive radii and iv
correspond to the quadrant with positive x-axis and y-axis values,
respectively (see the kinematic map in Figure 3).
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Byte-by-byte Description of file: table9.dat table1[23].dat
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Bytes Format Units Label Explanations
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1- 6 F6.2 arcsec Xpos x coordinate of the Voronoi bin center (1)
8- 13 F6.2 arcsec Ypos y coordinate of the Voronoi bin center
15- 20 F6.2 km/s Vel Stellar rotational velocity at (Xpos,Ypos)
22- 26 F5.2 km/s e_Vel Uncertainty in Vel
28- 33 F6.2 km/s sigma Stellar velocity dispersion σ
35- 39 F5.2 km/s e_sigma Uncertainty in sigma
41- 47 F7.4 --- h3 Gauss-Hermite moment, h3
49- 54 F6.4 --- e_h3 Uncertainty in h3
56- 62 F7.4 --- h4 Gauss-Hermite moment, h4
64- 69 F6.4 --- e_h4 Uncertainty in h4
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Note (1): The x-axis is aligned with the major axis.
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Byte-by-byte Description of file: table1[01].dat
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Bytes Format Units Label Explanations
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1- 4 F4.1 arcsec R Position within the slit (G1)
6- 9 F4.1 arcsec shift Slit shift from center (1)
11- 17 F7.2 km/s V(R) Stellar rotational velocity (relative to
V(0) fir NGC4751 or to average for NGC5516)
19- 24 F6.2 km/s e_V(R) Uncertainty in V(R)
26- 31 F6.2 km/s sigma Stellar velocity dispersion
33- 38 F6.2 km/s e_sigma Uncertainty in sigma
40- 45 F6.3 --- h3 Gauss-Hermite moment, h3
47- 51 F5.3 --- e_h3 Uncertainty in h3
53- 58 F6.3 --- h4 Gauss-Hermite moment, h4
60- 64 F5.3 --- e_h4 Uncertainty in h4
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Note (1): With respect to the center of the galaxy along the East (positive
shifts in arcsec) or West (negative shifts) directions.
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Global notes:
Note (G1): With positive radii indicating distances in arcsec from the center of
the slit towards the North and negative radii towards the South).
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 07-Jul-2014