Black Holes: Nobel Prize in Physics 2020 Julien Woillez (ESO) Nobel Prize in Physics 2020 Roger Penrose Reinhard Genzel & Andrea Ghez “for the discovery that black hole formation “for the discovery of a is a robust prediction supermassive compact of the general theory object at the centre of our of relativity” galaxy” Roger Penrose Reinhard Genzel Andrea Ghez ’60s Quasi Stellar Objects Very small, very far, ultra-luminous, and therefore very massive Schmidt 1963 3C 273 ESA/Hubble Picture of the Week Hubble 1929 ’60s Accretion disks and super massive black holes Electromagnetic radiation Accreting matter A very efficient central engine converts gravitational energy into EM radiation Salpeter 1964, Zeldovich & Novikov 1965 ’60s What about non-active galaxies, like ours? Is a starved supermassive black hole there? Lynden-Bell, 1969 Lynden-Bell & Rees, 1971 ’80s Unification of Active Galactic Nuclei All Active Galaxies have the same black and accretion disk central engine Broad emission lines in polarized light Antonucci & Miller, 1985 ’80s What about our galaxy? Galactic Center M87 No bright counterpart in Radio, X-ray, IR No jet M87 VLA EHT 2019 Owens, Biretta, Eilek ’80s Birth of infrared astronomy Wollman+77, Lacy, Townes, Hollenbach 82, … ’90s Near-IR astronomy at La Silla Observatory (Chile) Adaptive Optics (ESO 3.6m) Speckle Imaging (NTT 3.58 m) 3D spectroscopy (MPG/ESO 2.2 m) ’90s Speckle imaging Long exposures Short exposures ~10” ( 10 light years ) years light 10 ( ~10” Speckle imaging Weigelt 1977 http://www.mpifr-bonn.mpg.de/div/ir-interferometry/movie/speckle/specklemovie.html Labeyrie et al. 1974 ’90s Speckle imaging Eckart+ 1992 Eckart & Genzel 1997 ’90s 10-meter-class telescope era starts in the US Keck I first science in 1993 Keck II first light in 1996 ’90s First stellar orbits Ghez+ 1998 50 mas angular resolution Ghez+ 2000 ’90s Beyond the atmospheric turbulence limit Adaptive Optics COME-ON+, SHARPII, ADONIS Rigaut+, Beuzit+, Hubin+, Bonnacini+, Lacombes+, Brandl+, Eisenhauer+ Courtesy of ESO/L Calcada Clenet+01 ’90s Birth of Very Large Telescope First science between 1998 ~ 2000 ’00s Adaptive optics first light at Keck Observatory 1999: First light for Keck II Adaptive Optics Wizinowich+2000 2002 S2 a 15.2-year orbit around SgrA* Speckle imaging La Silla NTT Adaptive optics imaging Paranal VLT (NACO instrument) Schödel+ 2002 2002 (-16 years) The S2 count down S2 becomes the best test particle! 16 years to go 2002 2018 Schödel+ 2002 2002 (-16 years) Adaptive Optics and Spectroscopy Ghez+2003 Redshift gives radial velocity 2003 (-15 years) The variable IR counter part of SgrA* Genzel+2003 Ghez+2004 17 minutes period! 2004 (-14 years) Laser guide star Adaptive Optics Wizinowich+ 2006 Ghez+ 2005 Dancing stars SINFONI 18.08.04: K(75 mas) 0.6 21 22 NACO 10.06.04: H (40mas) 0.4 26 15 W6 S12 ) 0.2 9 S08 S5 arcsec * ( * S4 S14 S2 Astrometry S6 S13 Spectroscopy SgrA 0 S7 S7 S17 8 offset fromoffset -0.2 - 7 S1 Dec. S8 14.7 10 S9 19 -0.4 S9 S10 25 S013 16 0.5” (23 light days) S19 S11 23 -0.6 0.6 0.4 0.2 0 -0.2 -0.4 -0.6 R.A.-offset from SgrA* (arcsec) Schödel+02, Ghez+03,05,08, Eisenhauer+03,05, Paumard+07, Do+09, Gillessen+09,17, Meyer+12, Boehle+16, Fritz+16, Habibi+17 ... Gillessen+12,13,18, Phifer+14, Witzel+14, Pfuhl+15, Valencia-S.+15, Shahzamanian+16, Zajaček+17, Plewa+17 Dancing stars 2005 (-13 years) Better than adaptive optics: stellar interferometry GRAVITY instrument Project starts 2007 (-11 years) First light 2015 (-3 years) GRAVITY collaboration+ 2017 2006 (-12 years) Keck Interferometer / ASTRA Keck Interferometer was shut down in 2012 (-6 years) Woillez, Wizinowich+ 2014 2018 (-0 years) 1000x more sensitive than earlier interferometers 20-50 µas orbit precision June Motion of S2 seen from 3 day to day 1 30 27 24 Peri 19 May 4 2 28 26 April May/June 2018 May Moving at 8000 km/s 50 mas GRAVITY collaboration+18 Measurement of Gravitational Redshift Einstein GRAVITY collaboration+18 Newton Precise Measurement of Schwarzschild Precession Schwarzschild GRAVITY collaboration+20 o o 2 Jul 22 2018 flare, MJD=58321.9954 R=7 R a=0 i=160 =160 =1.2 g r 100 50 100 0 0 -50 Even Closer – Orbital Motion Close to the Last -100 -100 Stable Orbit -150 In 45 minutes100 round0 the black-100 hole 0 10 20 30 100.000 km/s = 30% speed of light ) c 100 2 e s ) c 2 r S a f ( o 100 t s e t ) i s 0 s f n f a u o ( ) n t 1 i d ( 0 e e s y r f t f ( i o y s - -100 n y d e n d a -100 ) x e u l f u l b ( -200 0 x 0 10 20 30 100 0 -100 time (mins) x-offset(as) GRAVITY collaboration+18 Mass of SgrA* Concentrated within few Schwarzschild Radii R/RS 1 10 102 103 104 105 106 107 old stars 107 clockwise disc flare S2 S-stars CND 106 5 10 Extended mass radio size upper limit 104 event horizon 103 enclosed (solar massmasses) 102 0.001 0.01 0.1 1 10 Radius (parsec) GRAVITY collaboration+18 Sensitivity, Sensitivity, Sensitivity, … Accuracy, Accuracy, Accuracy, … Contrast, Contrast, Contrast, … GRAVITY+ Faint All Sky Milli Arcsecond Imaging and Micro Arcsecond (Spectro) Astrometry KU Lueven.