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Jonelle Walsh (Texas A&M) TMT Science Forum Dec 10, 2018 Introduction: Black Holes Are Everywhere

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Jonelle Walsh (Texas A&M) TMT Science Forum Dec 10, 2018 Introduction: Black Holes Are Everywhere Exploring the Supermassive Black Hole - Galaxy Connection Jonelle Walsh (Texas A&M) TMT Science Forum Dec 10, 2018 Introduction: Black Holes are Everywhere Types of Black Holes ✦ Supermassive BHs reside in essentially every massive galaxy. Supermassive 1 billion 1 billion ✦ The strongest evidence we have for a BH Black Holes comes from the Milky Way (e.g., Genzel et al. 2010, Boehle et al. 2016). Supermassive Black Holes Supermassive 1 million (This image 1 million was created by Prof. Andrea Ghez and her research team at UCLA and are from Types of Black Holes Types data sets obtained 1000 with the W. 1000 black hole mass (relative to Sun) black hole mass (relative M. Keck Telescopes.) 100100 1010 Stellar-mass Black Holes Stellar-mass Stellar-mass 1 1 ✦ Beyond the Milky Way, BHs have been Black Holes black hole mass dynamically detected in ~100 galaxies (e.g., (M⊙) Saglia et al. 2016). Dynamical Searches for Black Holes ✦ Precise MBH measurements require high angular (HST) (credit: ESA/Hubble) resolution observations. ✦ Observations need to probe region over which the BH potential dominates — the BH sphere of influence (rsphere). ✦ Typical values for rsphere are small, so we are limited to studying nearby (~100 Mpc) objects. ✦ HST has played a fundamental role in detecting BHs over the past two decades. Dynamical Searches for Black Holes ✦ Significant progress has recently been made using large ground-based telescopes + AO (e.g., Mazzalay et (Keck) al. 2016, Erwin et al. 2018, Krajnović et al. 2018). ✦ ALMA also provides superb sensitivity and angular resolution high enough to directly detect molecular gas within rsphere (e.g., Barth et al. 2016, Onishi et al. 2017, Davis et al. 2017). (ALMA) (credit: Stephane Guisard/ESO) (credit: Laurie Hatch Photography http://www.lauriehatch.com/) Black Hole Mass Measurement Methods STELLAR DYNAMICS IONIZED GAS DISKS MASER DISKS ✦ Widely applicable, BUT●●● ✦ Conceptually simple, ✦ Produce some of the most BUT●●● precise MBH’s, BUT●●● ✦ Models are complex. ✦ Assumption of circular ✦ Disks are rare — they ✦ Models can be biased due rotation must be verified. require special physical to a number of systematic conditions and nearly edge- effects. ✦ Often the observed on inclinations. velocity dispersion is larger ‣ MBH - M/L - DM than that predicted from ✦ There can be significant degeneracies models. gravitational contributions ‣ intrinsic shape/ from disks themselves that orientation effects ‣ what is the physical lead to departures from origin and what does Keplerian rotation. that mean for MBH? (e.g., Gebhardt & Thomas 2009, van den (e.g., Barth et al. 2001, Verdoes Kleijn et (e.g., Miyoshi et al. 1995, Lodato & Bertin Bosch & de Zeeuw 2010, Rusli et al. 2013, al. 2006, Walsh et al. 2010) 2003, Pesce et al. 2015) McConnell et al. 2013) Black Hole Mass Measurement Methods STELLAR DYNAMICS IONIZED GAS DISKS MASER DISKS ✦ Widely applicable, BUT●●● ✦ Conceptually simple, ✦ Produce some of the most BUT●●● precise MBH’s, BUT●●● ✦ Models are complex. ✦ Assumption of circular ✦ Disks are rare — they ✦ Models can be biased due rotation must be verified. require special physical to a number of systematic conditions and nearly edge- effects. ✦ Often the observed on inclinations. velocity dispersion is larger ‣ MBH - M/L - DM than that predicted from ✦ There can be significant degeneracies models. gravitational contributions ‣ intrinsic shape/ from disks themselves that orientation effects ‣ what is the physical lead to departures from origin and what does Keplerian rotation. that mean for MBH? (e.g., Gebhardt & Thomas 2009, van den (e.g., Barth et al. 2001, Verdoes Kleijn et (e.g., Miyoshi et al. 1995, Lodato & Bertin Bosch & de Zeeuw 2010, Rusli et al. 2013, al. 2006, Walsh et al. 2010) 2003, Pesce et al. 2015) McConnell et al. 2013) Black Hole Mass Measurement Methods STELLAR DYNAMICS IONIZED GAS DISKS MASER DISKS ✦ Widely applicable, BUT●●● ✦ Conceptually simple, ✦ Produce some of the most BUT●●● precise MBH’s, BUT●●● ✦ Models are complex. ✦ Assumption of circular ✦ Disks are rare — they ✦ Models can be biased due rotation must be verified. require special physical to a number of systematic conditions and nearly edge- effects. ✦ Often the observed on inclinations. velocity dispersion is larger ‣ MBH - M/L - DM than that predicted from ✦ There can be significant degeneracies models. gravitational contributions ‣ intrinsic shape/ from disks themselves that orientation effects ‣ what is the physical lead to departures from origin and what does Keplerian rotation. that mean for MBH? (e.g., Gebhardt & Thomas 2009, van den (e.g., Barth et al. 2001, Verdoes Kleijn et (e.g., Miyoshi et al. 1995, Lodato & Bertin Bosch & de Zeeuw 2010, Rusli et al. 2013, al. 2006, Walsh et al. 2010) 2003, Pesce et al. 2015) McConnell et al. 2013) 6 6 6 6 A Stellar-Dynamical Black Hole Mass Measurement Example ✦ Stellar-dynamical measurements require high-angular resolution spectroscopy, high- angular resolutionFIG imaging,. 2.— Results and of stellar-dynamical large-scale models spectroscopy. fit to the NIFS kinematics. The χ2 is shown with black hole mass (left panel) and V-band mass-to-light ratio (middle panel). Each black dot corresponds to a single model, with the best-fit model highlighted as the red square. The red solid line indicates where ∆χ2 =9.0, corresponding to the 3σ confidence level for one parameter. χ2 contours are shown for a grid of black hole masses and mass-to-light ratios (right panel). Each 9 2 gray point represents a model, and the best-fit model (red square) corresponds to MBH =4.9 × 10 M⊙ and ΥV =9.3 Υ⊙. Relative to the minimum, the χ 2 hasFIG.F increased 2.—IG. 2.— Results by Results 2.3 of (thick stellar-dynamical of✦ stellar-dynamical black contour), models models 6.2 fit (thin to fit the black to NIFSthe contour), NIFS kinemat kinemat andics. 11.8ics. The (red Theχ2 contour),isχ shownis shown with corresponding with black black hole tohole mass the mass 1 (leftσ,2 (left panel)σ,and3 panel) andσ andconfidenceV-bandV-band mass-to-light intervals mass-to-light for ratio two ratio NGC 1277 Obtained Gemini/NIFS observations assisted by LGS ∆ 2 (middleparameters.(middle panel). panel). Each Each black black dot corresponds dot corresponds to a to single a single model, model, with w theith best-fit the best-fit model model highlighted highlighted as the as red the square. red square. The The red so redlid so linelid line indicates indicates where where∆χ2 =9χ .0,=9.0, 2 correspondingcorresponding to the to 3 theσ confidence 3σ confidenceAO. level The level for one forIFU one parameter. parameter.dataχ2 probescontoursχ contours are shown arethe shown for central a for grid a grid of black of ~1” black hole hole masses(340 masses and pc) and mass-to-l mass-to-l regionightight ratios ratios (right (right panel). panel). Each Each ×9 9 Υ Υ 2 2 graygray point point represents represents a model, a model, and and the best-fitthe best-fit model model (red (red squar square) correspondse) corresponds to M toBHM=4BH .=49 ×.910 10M⊙Mand⊙ andΥV =9V .=93 Υ.3⊙. Relative⊙. Relative to the to minimum,the minimum, the χ the χ hasFhas increasedIG. increased 2.— Results by 2.3 by (thick2.3 of stellar-dynamical (thick blackwith black contour), contour), a modelsPSF 6.2 (thin6.2 fit~0.15” (thin to black the black c NIFSontour), c.ontour), kinemat and and 11.8ics. 11.8 The (red (redχ contour),2 is contour), shown corresponding with corresponding black hole to the to mass 1theσ,2 (left 1σσ,2,and3 panel)σ,and3σ andconfidenceσVconfidence-band mass-to-light intervals intervals for two for ratio two parameters.(middleparameters. panel). Each black dot corresponds to a single model, with the best-fit model highlighted as the red square. The red solid line indicates where ∆χ2 =9.0, corresponding to the 3σ confidence level for one parameter. χ2 contours are shown for a grid of black hole masses and mass-to-light ratios (right panel). Each ✦ 9 2 gray point represents a model,Measured and the best-fit modelthe (redline-of-sight square) corresponds velocity to MBH =4 .9distribution× 10 M⊙ and ΥV =9(LOSVD).3 Υ⊙. Relative of to the minimum, the χ has increased by 2.3 (thick black contour), 6.2 (thin black contour), and 11.8 (red contour), corresponding to the 1σ,2σ,and3σ confidence intervals for two parameters. stars as a function of spatial location. LOSVD parameterized with V, σ, h 3, and h4. (Walsh et al. 2016) FIG. 3.— The observed NIFS kinematics (top) show that NGC 1277 is rotating, with the west side of the galaxy being blue-shifted,thatthereisasharprise in the velocity dispersion and generally positive h4 values at the nucleus, and that h3 and V are anti-correlated. The best-fit stellar dynamical model (bottom) is shown on the same scale given by the color bar to the right and the minimum/maximum values are provided at the top of the maps. The best-fit model nicely reproduces the NIFS observations and has a reduced χ2 of 0.7. FIG.F 3.—IG. 3.— The The observed observed NIFS NIFS kinematics kinematics (top) (top) show show that that NGC NGC 1277 1277 is rotating, is rotating, with with the west the west side side of the of galaxy the galaxy being being blue-shifted blue-shifted,thatthereisasharprise,thatthereisasharprise h h V in thein velocity the velocity dispersion dispersion and and generally generally positive positiveh4 values4 values at the at nucleus, the nucleus, and and that thath3 and3 andV are anti-correlated.are anti-correlated. The The best-fit best-fit stellar stellar dynamical dynamical model model (bottom) (bottom) is is shownitedshown mass on the on degeneracies samethe same scale scale given given with by the by the colorthe galaxy’s color bar barto the dark to rightthe halo right and (e.g.,and the minimum/maximumthe Ge minimum/maximumb- Shapiro values values et are al.
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