STELLAR DYNAMICS IN THE NUCLEI OF M31 AND M32: EVIDENCE FOR MASSIVE BLACK HOLES A LAN D RESSLER

Transcription

1 STELLAR DYNAMICS IN THE NUCLEI OF M31 AND M32: EVIDENCE FOR MASSIVE BLACK HOLES A LAN D RESSLER

2 ABSTRACT 이웃하는두은하인 M32, M32 의중심에거대블랙홀이있는것같다!! Ca II M31, M32, maximum entropy technique 3 2 M31, M32 M/L masses (3 7) 10 7, solar 10 9 solar masses, quasar 2

3 CONTENTS INTRODUCTION 1 2 DYNMICAL MODELS AND COMPARISON WITH THE DATA 3 4 DISCUSSION DATA AND ANALYSIS 3

4 I. INTRODUCTION M31, M32 중심부의회전속도가빠른것은이전연구들에서꾸준히제기되어왔다. 우리는더높은신호대잡음비를갖는최신의데이터로부터새로운동역학적모델을제시한다. 그리고그결과두은하의중심에는거대블랙홀이있다는결론에도달했다. Pioneering observations of M31 by Walker, Lallemand, Duchesne (1960) and M32 by Walker (1962) found rapid rotation of the stellar systems in both nuclei. Later studies of M32 by Tonry (1984) and Dressier (1984) and of M31 by Dressier (1984) and Kormendy (1987) confirmed abrupt rises in the stellar rotation rates as well as sharp increases in the apparent velocity dispersions of both these systems. This paper presents new data on both M31 and M32 that in signal-to-noise ratio and spatial resolution are superior to the data of the earlier studies and the equal of any now available. Using new dynamical models, we determine the mass distribution of the centers of these galaxies with much greater reliability than in the past. There is no question that the nuclei have very large mass-to-light ratios, recalling, in the case of M31, model A of Ostriker and Tremaine (1982). Our results strongly suggest the presence of massive black holes in the nuclei of both galaxies. 4

5 II. DATA AND ANALYSIS a.the Data b.m32 c.m31 5

6 1. DATA 2. M32 3. M31 CA II TRIPLET AT 8498, 8542, AND 8662  Using the double spectrograph on the 5 m Hale telescope at Palomar Observatory The instrument was configured to sample the and  regions with two Texas Instruments 800 x 800 CCDs. The sampling was ~1.1  per pixel in the blue and ~0.8  per pixel in the infrared. The observations were made with a 1"0 slit which resulted in instrumental FWHM widths of 2.2 and 1.6 Â, which correspond to velocity widths a = 51 km s-1 and 25 km s-1, respectively Two consecutive exposures of M32 and three consecutive exposures of M31 of 500 s duration were made, each aligned along the major axis. The errors in systemic velocity v and σ are very small, so there can be no doubt as to the reality of the apparent rise of the velocity dispersion to ~84 km s-1 and a rotation gradient of at least 40 km s-1 arcsec-1 (1 arc second = 3.35 pc) kinematical structure with an semiamplitude of ~100 km s-1. The velocity dispersion appears to increase from ~140 km s_1 to over 220 km s-1. the kinematic center is displaced from the luminosity peak by 0."50

7 III. DYNAMICAL MODELS AND COMPARISON WITH THE DATA a.dynamical Models b.simulating Data c.the Modelfor M32 d.the Modelfor MSI 7

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9 IV. DISCUSSION M31, M32 중심부의회전속도가빠른것은이전연구들에서꾸준히제기되어왔다. 우리는더높은신호대잡음비를갖는최신의데이터로부터새로운동역학적모델을제시한다. 그리고그결과두은하의중심에는거대블랙홀이있다는결론에도달했다. Pioneering observations of M31 by Walker, Lallemand, Duchesne (1960) and M32 by Walker (1962) found rapid rotation of the stellar systems in both nuclei. Later studies of M32 by Tonry (1984) and Dressier (1984) and of M31 by Dressier (1984) and Kormendy (1987) confirmed abrupt rises in the stellar rotation rates as well as sharp increases in the apparent velocity dispersions of both these systems. This paper presents new data on both M31 and M32 that in signal-to-noise ratio and spatial resolution are superior to the data of the earlier studies and the equal of any now available. Using new dynamical models, we determine the mass distribution of the centers of these galaxies with much greater reliability than in the past. There is no question that the nuclei have very large mass-to-light ratios, recalling, in the case of M31, model A of Ostriker and Tremaine (1982). Our results strongly suggest the presence of massive black holes in the nuclei of both galaxies. 9

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