An Hα dynamical mass for HE 0047–1756

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Publisher’s version / Version de l'éditeur:

Proceedings of the International Astronomical Union, 5, S267, pp. 205-205,

2009-08

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An Hα dynamical mass for HE 0047–1756

Inskip, K. J.; Jahnke, K.; Rix, H.-W.; Peng, C. Y.

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Co-Evolution of Central Black Holes and Galaxies Proceedings IAU Symposium No. 267, 2009

B. M. Peterson, R. S. Somerville, & T. Storchi-Bergmann, eds. c

International Astronomical Union 2010 doi:10.1017/S1743921310006253

An Hα Dynamical Mass for HE 0047−1756

K. J. Inskip

1

, K. Jahnke

1

, H.-W. Rix

1

, and C. Y. Peng

2

1_{Max-Planck-Institut f¨}_{ur Astronomie, K¨}_{onigstuhl 17, D-69117 Heidelberg, Germany}

Email: inskip, jahnke, rix@mpia.de

2_{Herzberg Institute of Astrophysics, National Research Council of Canada,}

5071 West Saanich Rd., Victoria, BC V9E 2E7, Canada Email: cyp@nrc-cnrc.gc.ca

Abstract.We derive Mb u lg e for HE 0047−1756 via Hα gas dynamics. The resulting large value

of MB H/Mb u lg e may imply evolution in the correlation at high redshifts.

Keywords.galaxies: active, galaxies: evolution, quasars: individual (HE 0047−1756)

We have obtained AO-IFU spectroscopy of the gravitationally lensed z = 1.66 QSO

HE 0047−1756 (Figure 1a) using SINFONI (Eisenhauer et al. 2003, Bonnet et al. 2004).

After successful removal of the strong QSO emission, we locate and model the host

galaxy’s narrow Hα emission. The resulting velocity ﬁeld (Figure 1b) is consistent with

ordered rotation; applying the lensing model for this source (Peng et al. 2006) implies a

dynamical mass of M

bulge

∼ 6.5 × 10

10

M

⊙

. Together with a measured value of M

BH

=

1.48×10

9

M

⊙

(Peng et al. 2006), we include HE 0047−1756 on the nearby galaxy M

BH

vs.

M

bulge

relation of H¨

aring & Rix (2004) (Figure 1c). Our derived mass, although somewhat

small, is comparable to some other high-z CO-based measurements (e.g., Riechers et al.

2008). Overall, these results favor evolution in the ratio M

BH

/M

bulge

, with massive black

holes existing in relatively less massive host galaxies at earlier cosmic epochs.

References

Bonnet, H., et al. 2004, The ESO Messenger, 117, 17 Eisenhauer, F., et al. 2003, SPIE 4841, 1548

H¨aring, N., Rix H.-W. 2004, ApJ, 604, L89

Peng, C. Y., Impey, C. D., Rix, H.-W., Kochanek, C. S., Keeton, C. R., Falco, E. E., Leh´ar, J., & McLeod, B. A. 2006, ApJ, 649, 616

Riechers, D. A., Walter, F., Brewer, B. J., Carilli, C. L., Lewis, G. F., Bertoldi, F., & Cox, P., 2008, ApJ, 686, 851

Figure 1.Left:Median data cube image. Center: Hα velocity ﬁeld (velocities in km s−1_).

Right:MB H vs. Mb u lg e relation (H¨aring & Rix 2004) including HE 0047−1756 (large star).

205

available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S1743921310006253