2 July 2018 Toshinori Hayashi. Discovery of an Extraordinary Binary System

Size: px
Start display at page:

Download "2 July 2018 Toshinori Hayashi. Discovery of an Extraordinary Binary System"

Transcription

1 2 July 2018 Toshinori Hayashi CONTENTS 1. arxiv: v1[astro-ph.he] 7 Jun 2018, Todd A. Thompson et al. Discovery of an Extraordinary Binary System 2. MNRAS 475, L15-L19 (2018) doi: /mnrasl/slx203 A detached stellar-mass black hole candidate in the globular cluster NGC 3201

2 Common introduction How to observe detached binaries including unseen objects X-ray binary(wikipedia) GW from a BH merger (Wikipedia)

3 2 4 M M e 0 P days? Non interacting -no accretion disk(noxray) Almost circular - e = ± Massive companion - a NS or a black hole?

4 : APOGEE > 10 B star in Galaxy a ΔRV Δt IJ K LMN 200 sources with highest acceleration. ASAS-SN Search for periodic photometric variations Transits, ellipsoidal variations, or starspots

5 2M l, b = , Acceleration a 2.9 km s YZ day YZ Photometric variation P [\1] days APOGEE spectrum analysis v sin i b1] 14.1 ± 0.6 kms YZ T dee 4480 ± 62K Well-fit by a single reddened template

6 TRES Best fit parameters P = ± days e = ± K = ± kms YZ f M M ij k sin k i 1b2 p M lmmn] + M ij = ± M

7 Assume that this system is tidally synchronized and circularized. i b1] = i 1b2 = i P b1] = P 1b2 = P v sin i 14.1 kms YZ R 23R / sin i L 200L / sin p i D 2.4 kpc/ sin i From Gaia parallax data s D 3.7 ± 0.8 kpc R 36 ± 8 R L 480 ± 100 L sin i 0.64 ± 0.14 L

8 With the constraint log g = 2.35 ± 0.14 from TRES L, R, T dee from Gaia and SED.ƒ M lmmn] = 3.0 Y.B M 1σ log g = 2.2 ± 0.1 Zp L = 290 Yk L Zƒ T dee = 4890 YZ K k. R = 23.8 Y.ƒ R Age = 10.B±.p Myr. p sin i = 0.97 Y.Z Z.Z M ij = 3.2 Y. M

9 log g Different analysis of spectra give different log g log g = 2.59 ± APOGEE log g = 2.2 APOGEE, lowest report log g = 2.35 ± 0.14 TRES log g might have a large systematic uncertasinty due to rapid rotation, spots, red colors? Best fitting without constraint log g Z.p M lmmn] = 2.2 Y. M 1σ pk L = 480 YZ L T dee = 4510 Ypp K.k R = 35.8 Y.ƒ R.Z sin i = 0.65 Y.Zp M ij = 5.5 Yp.p Looks match well but.p log g = 1.7 Y.k too small k.p M

10 Stars on the giant branch normally exhibit a negative correlation between [C/N] and mass, due to nuclear process. 2M may be an outlier. Due to binary interaction or previous merger in a triple system?

11 cluster NGC 3201 Non interacting - no accretion disk(no Xray) > 4.36 M? e 0.6 ~0.8 M P days Highly eccentric - e = ± Massive companion - Likely a black hole? In a globular cluster

12 Blue square: the star for reference Red cross-hairs: the object reported in this paper MUSE spectroscopy Spatial resolution 1800 < R < 3500 of some thousands stars per exposure Identified 3 stars with RV variations exceeding 100 kms YZ. One of them can be analysed. Other two need more observation.

13 Target star RA: 10 \ 17 L Dec No significant variations in magnitude No pulsation indicates RV is not due to star-intrinsic Compare NGC 3201 HST ACS CMD(Colour Magnitude Diagram) and PARSEC isochrone Best fit parameters M = 0.81 ± 0.05 M T dee = 6126 ± 20 K log g = 3.99 ± 0.05 dex M/H = 1.50 ± 0.02 dex

14 All radial velocity corrected spectra Red: Best fit PHOENIX spectra Fitting Göttingen Spectral Library of Synthetic PHOENIX spectra T dee = 6126 ± 20 K M/H = 1.50 ± 0.02 dex No emission lines indicating a cataclysmic variable or a compact binary with an illuminated low-mass star and a hot companion like a WD or NS Radial Velocity

15 Black: circular Red: Full Keplerian fit Generalized Lomb-Scargle periodgram Using likelihood function to find periodicity 167 days periodicity is likely. Phase folding & fitting RV K = 69.4 ± 2.5 kms YZ e = ± M sin i = 4.36 ± 0.41 M a M = 1.03 ± 0.03 au Companion may be a BH?

16 2M 2? a NS binary? Possibly a triple star system that consists of a compact double NS binary with a MS turn off around it But such a system never observed & actual mass of the discovered object may be higher a BH scenario is more likely?

Optical studies of an ultraluminous X-ray source: NGC1313 X-2

Optical studies of an ultraluminous X-ray source: NGC1313 X-2 Optical studies of an ultraluminous X-ray source: NGC1313 X-2 Jifeng Liu Harvard-Smithsonian Center for Astrophysics in collaboration with Joel Bregman, Jon Miller, Philip Kaaret outline background: ultraluminous

More information

Accretion in Binaries

Accretion in Binaries Accretion in Binaries Two paths for accretion Roche-lobe overflow Wind-fed accretion Classes of X-ray binaries Low-mass (BH and NS) High-mass (BH and NS) X-ray pulsars (NS) Be/X-ray binaries (NS) Roche

More information

A RADIO SEARCH FOR BLACK HOLES IN THE MILKY WAY GLOBULAR CLUSTER M10

A RADIO SEARCH FOR BLACK HOLES IN THE MILKY WAY GLOBULAR CLUSTER M10 (nrao/aui) LAURA SHISHKOVSKY, J. STRADER, L. CHOMIUK, L. TREMOU (MSU), J. MILLER-JONES, V. TUDOR (CURTIN), T. MACCARONE (TEXAS TECH), G. SIVAKOFF, C. HEINKE (U. ALBERTA) A RADIO SEARCH FOR BLACK HOLES

More information

Kozai-Lidov oscillations

Kozai-Lidov oscillations Kozai-Lidov oscillations Kozai (1962 - asteroids); Lidov (1962 - artificial satellites) arise most simply in restricted three-body problem (two massive bodies on a Kepler orbit + a test particle) e.g.,

More information

Gaia News:Counting down to launch A. Vallenari. INAF, Padova Astronomical Observatory on behalf of DPACE

Gaia News:Counting down to launch A. Vallenari. INAF, Padova Astronomical Observatory on behalf of DPACE Gaia News:Counting down to launch A. Vallenari INAF, Padova Astronomical Observatory on behalf of DPACE Outline Gaia Spacecraft status The Gaia sky Gaia open and globular clusters From data to science:

More information

FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS

FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS Main Categories of Compact Systems Formation of Compact Objects Mass and Angular Momentum Loss Evolutionary Links to Classes of Binary Systems Future Work

More information

Announcement: Quiz Friday, Oct 31

Announcement: Quiz Friday, Oct 31 Announcement: Quiz Friday, Oct 31 What is the difference between the giant, horizontal, and asymptotic-giant branches? What is the Helium flash? Why can t high-mass stars support themselves in hydrostatic

More information

Hot-subdwarf stars: a new class of X-ray sources

Hot-subdwarf stars: a new class of X-ray sources Hot-subdwarf stars: a new class of X-ray sources Nicola La Palombara 1 S. Mereghetti 1, A. Tiengo 1,2,3, P. Esposito 1 1 INAF - IASF Milano, 2 IUSS Pavia, 3 INFN Pavia Dublin June 16-19, 2014 Hot subdwarf

More information

Building the cosmic distance scale: from Hipparcos to Gaia

Building the cosmic distance scale: from Hipparcos to Gaia The Fundamental Distance Scale: state of the art and the Gaia perspectives 3-6 May 2011 Building the cosmic distance scale: from Hipparcos to Gaia Catherine TURON and Xavier LURI 1 ESA / ESO-H. Heyer Fundamental

More information

Identification of compact objects in X-ray/gamma-ray binaries and the exploration of long-period exoplanets by high-precision astrometry

Identification of compact objects in X-ray/gamma-ray binaries and the exploration of long-period exoplanets by high-precision astrometry X-ray binary Gaia Gaia-JASMINE Joint Meeting @NAOJ, 6-9 Dec. 2016 exoplanet ESA/ATG NAOJ Identification of compact objects in X-ray/gamma-ray binaries and the exploration of long-period exoplanets by high-precision

More information

Astronomy 100 Spring 2006 Lecture Questions Twelve Weeks Review

Astronomy 100 Spring 2006 Lecture Questions Twelve Weeks Review Astronomy 100 Spring 2006 Lecture Questions Twelve Weeks Review 16-1 Fusion in the Sun The solar corona has temperatures roughly the same as temperatures in the Sun's core, where nuclear fusion takes place.

More information

White dwarf populations. Gijs Nelemans Radboud University Nijmegen

White dwarf populations. Gijs Nelemans Radboud University Nijmegen White dwarf populations Gijs Nelemans Radboud University Nijmegen Outline Introduction: Population synthesis Basic ingredients Observational inputs White dwarf populations Different types and mergers WD

More information

Pulsars ASTR2110 Sarazin. Crab Pulsar in X-rays

Pulsars ASTR2110 Sarazin. Crab Pulsar in X-rays Pulsars ASTR2110 Sarazin Crab Pulsar in X-rays Test #2 Monday, November 13, 11-11:50 am Ruffner G006 (classroom) Bring pencils, paper, calculator You may not consult the text, your notes, or any other

More information

A Be-type star with a black hole companion

A Be-type star with a black hole companion A Be-type star with a black hole companion Jorge Casares (IAC) I. Negueruela (UA) M. Ribó (UB) I. Ribas (IEEC, CSIC) J.M. Paredes (UB) A. Herrero (IAC) S. Simón-Díaz (IAC) Nature 505 387 (2014; 16 Dec)

More information

Other planetary systems

Other planetary systems Exoplanets are faint! Other planetary systems Planets are seen only by reflected light at optical wavelengths At the distance of another star the faint light of a planet is lost in the glare of the star

More information

The SWARMS Survey: Unveiling the Galactic population of Compact White Dwarf Binaries

The SWARMS Survey: Unveiling the Galactic population of Compact White Dwarf Binaries The SWARMS Survey: Unveiling the Galactic population of Compact White Dwarf Binaries Weizmann Institute of Science / Tel-Aviv University Type Ia SN Progenitors Workshop Leiden, September 22 2010 Steve

More information

Can black holes be formed in dynamic interactions in star clusters?

Can black holes be formed in dynamic interactions in star clusters? Can black holes be formed in dynamic interactions in star clusters? Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences Warsaw, Poland mig@camk.edu.pl MODEST 14 Workshop Bad Honnef, Germany

More information

Demographics of radio galaxies nearby and at z~0.55. Are radio galaxies signposts to black-hole mergers?

Demographics of radio galaxies nearby and at z~0.55. Are radio galaxies signposts to black-hole mergers? Elaine M. Sadler Black holes in massive galaxies Demographics of radio galaxies nearby and at z~0.55 Are radio galaxies signposts to black-hole mergers? Work done with Russell Cannon, Scott Croom, Helen

More information

Binary sources of gravitational waves

Binary sources of gravitational waves Binary sources of gravitational waves For our final two lectures we will explore binary systems in general and the Advanced LIGO detections in particular. Binaries obviously have a large and varying quadrupole

More information

Dr. Reed L. Riddle. Close binaries, stellar interactions and novae. Guest lecture Astronomy 20 November 2, 2004

Dr. Reed L. Riddle. Close binaries, stellar interactions and novae. Guest lecture Astronomy 20 November 2, 2004 Dr. Reed L. Riddle Close binaries, stellar interactions and novae Guest lecture Astronomy 20 November 2, 2004 Gravitational Tides Look at the forces acting on one body orbiting another - more pull on closer

More information

Galaxies. Galaxy Diversity. Galaxies, AGN and Quasars. Physics 113 Goderya

Galaxies. Galaxy Diversity. Galaxies, AGN and Quasars. Physics 113 Goderya Galaxies, AGN and Quasars Physics 113 Goderya Chapter(s): 16 and 17 Learning Outcomes: Galaxies Star systems like our Milky Way Contain a few thousand to tens of billions of stars. Large variety of shapes

More information

Names: Team: Team Number:

Names: Team: Team Number: Astronomy C Michigan Region 8 March 11, 2017 Names: Team: Team Number: Directions 1. There is a separate answer sheet. Answers written elsewhere (e.g. on the test) will not be considered. 2. You may take

More information

Population of BHs in the Galaxy and in the MCs

Population of BHs in the Galaxy and in the MCs Population of BHs in the Galaxy and in the MCs INVENTORY OF GALACTIC BHs 1 SUPERMASSIVE BH (Sgr A*) (zero few tens?) of INTERMEDIATE MASS BHs 10 7 10 8 STELLAR MASS BHs From orbits (astrometry & spectroscopy)

More information

Eclipsing Binary Star studies: Present and future

Eclipsing Binary Star studies: Present and future Eclipsing Binary Star studies: Present and future P. G. iarchos Department of Astrophysics, Astronomy and Mechanics, ational and Kapodistrian University of Athens, Greece Abstract The importance of Eclipsing

More information

Techniques for measuring astronomical distances generally come in two variates, absolute and relative.

Techniques for measuring astronomical distances generally come in two variates, absolute and relative. Chapter 6 Distances 6.1 Preliminaries Techniques for measuring astronomical distances generally come in two variates, absolute and relative. Absolute distance measurements involve objects possibly unique

More information

Black Hole Binary System. Outline - Feb. 25, Constraining the Size of the Region that Contains the Invisible Mass

Black Hole Binary System. Outline - Feb. 25, Constraining the Size of the Region that Contains the Invisible Mass Outline - Feb. 25, 2010 Black Hole Binary System Observational evidence for Black Holes (pgs. 600-601) Properties of Stars (Ch. 16) Luminosities (pgs. 519-523) Temperatures (pg. 524) Optical image of Cygnus

More information

Page # Astronomical Distances. Lecture 2. Astronomical Distances. Cosmic Distance Ladder. Distance Methods. Size of Earth

Page # Astronomical Distances. Lecture 2. Astronomical Distances. Cosmic Distance Ladder. Distance Methods. Size of Earth Size of Astronomical istances ecture 2 Astronomical istances istance to the Moon (1 sec) istance to the Sun (8 min) istance to other stars (years) istance to centre of our Galaxy ( 30,000 yr to centre)

More information

Neutron Stars. Properties of Neutron Stars. Formation of Neutron Stars. Chapter 14. Neutron Stars and Black Holes. Topics for Today s Class

Neutron Stars. Properties of Neutron Stars. Formation of Neutron Stars. Chapter 14. Neutron Stars and Black Holes. Topics for Today s Class Foundations of Astronomy 13e Seeds Phys1403 Introductory Astronomy Instructor: Dr. Goderya Chapter 14 Neutron Stars and Black Holes Cengage Learning 2016 Topics for Today s Class Neutron Stars What is

More information

Synergy between MOSAIC, MICADO, and MUSE:

Synergy between MOSAIC, MICADO, and MUSE: Synergy between MOSAIC, MICADO, and MUSE: resolved stellar populations in nearby galaxies Martin M. Roth (P.I.) Andreas Kelz Leibniz-Institute for Astrophysics Potsdam (AIP) University of Potsdam Toledo,

More information

Milky Way s Anisotropy Profile with LAMOST/SDSS and Gaia

Milky Way s Anisotropy Profile with LAMOST/SDSS and Gaia Milky Way s Anisotropy Profile with LAMOST/SDSS and Gaia Shanghai Astronomical Observatory In collaboration with Juntai Shen, Xiang Xiang Xue, Chao Liu, Chris Flynn, Chengqun Yang Contents 1 Stellar Halo

More information

7. BINARY STARS (ZG: 12; CO: 7, 17)

7. BINARY STARS (ZG: 12; CO: 7, 17) 7. BINARY STARS (ZG: 12; CO: 7, 17) most stars are members of binary systems or multiple systems (triples, quadruples, quintuplets,...) orbital period distribution: P orb = 11 min to 10 6 yr the majority

More information

6. Detached eclipsing binaries

6. Detached eclipsing binaries Rolf Kudritzki SS 2015 6. Detached eclipsing binaries 50% of all stars live in binary systems and some of them are eclipsing 1 Rolf Kudritzki SS 2015 classification of binary systems by geometry of equipotential

More information

Galactic archaeology with the RAdial Velocity Experiment

Galactic archaeology with the RAdial Velocity Experiment Galactic archaeology with the RAdial Velocity Experiment Georges Kordopatis & RAVE collaboration Leibniz-Institute for Astrophysics, Potsdam Multi-Object Spectroscopy in the next decade: Big questions,

More information

Observing the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics

Observing the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics Observing the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics with: Tim Heckman (JHU) GALEX Science Team (PI: Chris Martin), Lee Armus,

More information

Chapter 14 The Milky Way Galaxy

Chapter 14 The Milky Way Galaxy Chapter 14 The Milky Way Galaxy Spiral Galaxy M81 - similar to our Milky Way Galaxy Our Parent Galaxy A galaxy is a giant collection of stellar and interstellar matter held together by gravity Billions

More information

Milky Way S&G Ch 2. Milky Way in near 1 IR H-W Rixhttp://online.kitp.ucsb.edu/online/galarcheo-c15/rix/

Milky Way S&G Ch 2. Milky Way in near 1 IR   H-W Rixhttp://online.kitp.ucsb.edu/online/galarcheo-c15/rix/ Why study the MW? its "easy" to study: big, bright, close Allows detailed studies of stellar kinematics, stellar evolution. star formation, direct detection of dark matter?? Milky Way S&G Ch 2 Problems

More information

Milky Way star clusters

Milky Way star clusters Using Γα ια for studying Milky Way star clusters Eugene Vasiliev Institute of Astronomy, Cambridge MODEST-, 26 June Overview of Gaia mission Scanning the entire sky every couple of weeks Astrometry for

More information

Pulsars as probes for the existence of IMBHs

Pulsars as probes for the existence of IMBHs Universidad de Valencia 15 November 2010 Pulsars as probes for the existence of IMBHs ANDREA POSSENTI Layout Known Black Hole classes Formation scenarios for the IMBHs IMBH candidates IMBH candidates (?)

More information

Chemistry & Dynamics of the Milky Way From Before Hipparcos Until Gaia

Chemistry & Dynamics of the Milky Way From Before Hipparcos Until Gaia Chemistry & Dynamics of the Milky Way From Before Hipparcos Until Gaia J. Andersen 1,2, B. Nordström 1,2 1 Dark Cosmology Centre, The Niels Bohr Institute, University of Copenhagen, Denmark 2 Stellar Astrophysics

More information

Recent Progress on our Understanding of He-Dominated Stellar Evolution

Recent Progress on our Understanding of He-Dominated Stellar Evolution Institute for Astronomy andastrophysics Recent Progress on our Understanding of He-Dominated Stellar Evolution 21.08.2015, N. Reindl Introduction H-deficient stars C-rich He ~ 30-50% C ~ 30-60% O ~ 2-20%

More information

Stellar mass black holes in young massive and open clusters and their role in gravitational-wave generation

Stellar mass black holes in young massive and open clusters and their role in gravitational-wave generation Stellar mass black holes in young massive and open clusters and their role in gravitational-wave generation Sambaran Banerjee Argelander-Institut für Astronomie (AIfA) and Helmholtz-Instituts für Strahlen-

More information

Black Hole Subsystems in Galactic Globular Clusters: Unravelling BH Populations in GCs using MOCCA Star Cluster Simulations

Black Hole Subsystems in Galactic Globular Clusters: Unravelling BH Populations in GCs using MOCCA Star Cluster Simulations Black Hole Subsystems in Galactic Globular Clusters: Unravelling BH Populations in GCs using MOCCA Star Cluster Simulations Artist impression of a stellar mass BH detected in NGC 3201 (Giesers et al. 2018)

More information

PoS(extremesky2009)103

PoS(extremesky2009)103 The study of the nature of sources AX J1749.1 2733 and AX J1749.2 2725 D. I. Karasev Space Research Institute, Profsoyuznaya str. 84/32, Moscow 117997, Russia E-mail: dkarasev@iki.rssi.ru Space Research

More information

Observations of extrasolar planets

Observations of extrasolar planets Observations of extrasolar planets 1 Mercury 2 Venus radar image from Magellan (vertical scale exaggerated 10 X) 3 Mars 4 Jupiter 5 Saturn 6 Saturn 7 Uranus and Neptune 8 we need to look out about 10 parsecs

More information

Open problems in compact object dynamics

Open problems in compact object dynamics Open problems in compact object dynamics Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund University www.astro.lu.se Key ideas and open questions in compact object dynamics Melvyn

More information

Asterseismology and Gaia

Asterseismology and Gaia Asterseismology and Gaia Asteroseismology can deliver accurate stellar radii and masses Huber et al 2017 compare results on distances from Gaia and asteroseismology for 2200 Kepler stars Asteroseismology

More information

Agenda for Ast 309N, Sep. 27. Measuring Masses from Binary Stars

Agenda for Ast 309N, Sep. 27. Measuring Masses from Binary Stars Agenda for Ast 309N, Sep. 27 Quiz 3 The role of stellar mass Ages of star clusters Exam 1, Thurs. Oct. 4 Study guide out on 9/28 Next topic: brown dwarfs and extrasolar planets 1 This image of the central

More information

Black holes in dormant X-ray transients

Black holes in dormant X-ray transients Mem. S.A.It. Vol. 83, 213 c SAIt 2012 Memorie della Black holes in dormant X-ray transients J. Ziółkowski Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warszawa, Poland e-mail: jz@camk.edu.pl

More information

Chapter 14. Outline. Neutron Stars and Black Holes. Note that the following lectures include. animations and PowerPoint effects such as

Chapter 14. Outline. Neutron Stars and Black Holes. Note that the following lectures include. animations and PowerPoint effects such as Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). Chapter 14 Neutron

More information

COSMOLOGY PHYS 30392 OBSERVING THE UNIVERSE Part I Giampaolo Pisano - Jodrell Bank Centre for Astrophysics The University of Manchester - January 2013 http://www.jb.man.ac.uk/~gp/ giampaolo.pisano@manchester.ac.uk

More information

JINA Observations, Now and in the Near Future

JINA Observations, Now and in the Near Future JINA Observations, Now and in the Near Future Timothy C. Beers Department of Physics & Astronomy Michigan State University & JINA: Joint Institute for Nuclear Astrophysics Examples SDSS-I, II, and III

More information

What have we learned from the detection of gravitational waves? Hyung Mok Lee Seoul National University

What have we learned from the detection of gravitational waves? Hyung Mok Lee Seoul National University What have we learned from the detection of gravitational waves? Hyung Mok Lee Seoul National University Outline Summary of 1st and 2nd Observing Runs Characteristics of detected sources Astrophysical Implications

More information

The Thousand Parsec Open Cluster Survey establishing new benchmarks for star and planet evolu7on

The Thousand Parsec Open Cluster Survey establishing new benchmarks for star and planet evolu7on The Thousand Parsec Open Cluster Survey establishing new benchmarks for star and planet evolu7on Russel White (Georgia State University) With advice/insight from: Lynne Hillenbrand (Caltech) Sam Quinn

More information

Raven Eyes Elliptical Galaxies and Star Clusters. T. J. Davidge November 24, 2015

Raven Eyes Elliptical Galaxies and Star Clusters. T. J. Davidge November 24, 2015 Raven Eyes Elliptical Galaxies and Star Clusters T. J. Davidge November 24, 2015 Why Maffei1 and the Glimpse Clusters? Targets were selected at low Galactic latitudes to maximize chances of finding a suitable

More information

Outline. Go over AGN problem, again, should be rotating BH Go over problem 6.6 Olber's paradox Distances Parallax Distance ladder Direct checks

Outline. Go over AGN problem, again, should be rotating BH Go over problem 6.6 Olber's paradox Distances Parallax Distance ladder Direct checks Outline Go over AGN problem, again, should be rotating BH Go over problem 6.6 Olber's paradox Distances Parallax Distance ladder Direct checks Why is the night sky dark? (Olber s Paradox 1826) Or what

More information

Special Relativity. Principles of Special Relativity: 1. The laws of physics are the same for all inertial observers.

Special Relativity. Principles of Special Relativity: 1. The laws of physics are the same for all inertial observers. Black Holes Special Relativity Principles of Special Relativity: 1. The laws of physics are the same for all inertial observers. 2. The speed of light is the same for all inertial observers regardless

More information

Globular Clusters in LSB Dwarf Galaxies

Globular Clusters in LSB Dwarf Galaxies Globular Clusters in LSB Dwarf Galaxies New results from HST photometry and VLT spectroscopy Thomas H. Puzia Herzberg Institute of Astrophysics in collaboration with Margarita E. Sharina SAO, Russian Academy

More information

SUPER STAR CLUSTERS: High Resolution Observations. James R. Graham (UCB) Nate McCrady (UCLA) & Andrea Gilbert (LLNL) KIPT

SUPER STAR CLUSTERS: High Resolution Observations. James R. Graham (UCB) Nate McCrady (UCLA) & Andrea Gilbert (LLNL) KIPT SUPER STAR CLUSTERS: High Resolution Observations James R. Graham (UCB) Nate McCrady (UCLA) & Andrea Gilbert (LLNL) KIPT 2007-8-16 M82 N 100 pc McCrady & Graham 2007 ACS F814W & NICMOS F160W/F222M images

More information

The Extragalactic Distance Scale

The Extragalactic Distance Scale One of the important relations in Astronomy. It lets us Measure the distance to distance objects. Each rung on the ladder is calibrated using lower-rung calibrations. Distance Objects Technique 1-100 AU

More information

Compact Binaries - 3 ASTR2110 Sarazin

Compact Binaries - 3 ASTR2110 Sarazin Compact Binaries - 3 ASTR2110 Sarazin Zoology of Binary Stars X-ray Binary Pulsar Spin-Up Accreted material has high angular momentum Spins up neutron star (true of ~all X-ray binary pulsars) Millisecond

More information

XRBs in Star-forming Galaxies X-ray Luminosity Functions Ultra-Luminous X-ray Sources

XRBs in Star-forming Galaxies X-ray Luminosity Functions Ultra-Luminous X-ray Sources XRBs in Star-forming Galaxies X-ray Luminosity Functions Ultra-Luminous X-ray Sources G. Fabbiano Harvard-Smithsonian CfA XRB Populations in Nearby Galaxies External galaxies provide `cleaner samples Distances

More information

The so-called final parsec problem

The so-called final parsec problem The so-called final parsec problem most galaxies contain black holes at their centers black-hole mass is 10 6-10 10 solar masses or roughly 0.2-0.5% of the stellar mass of the host galaxy galaxies form

More information

Determination of [α/fe] and its Application to SEGUE F/G Stars. Young Sun Lee

Determination of [α/fe] and its Application to SEGUE F/G Stars. Young Sun Lee Determination of [α/fe] and its Application to SEGUE F/G Stars Young Sun Lee Research Group Meeting on June 16, 2010 Outline Introduction Why [α/fe]? Determination of [α/fe] Validation of estimate of [α/fe]

More information

ASTR-101 4/4/2018 Stellar Evolution: Part II Lecture 19

ASTR-101 4/4/2018 Stellar Evolution: Part II Lecture 19 ASTR-101 4/4/2018 Stellar Evolution: Part II Lecture 19 WHEN S THE NEXT TEST?!?!?!? If anyone is following the syllabus, you know that it says there is a test today. The test will be on April 11 th (a

More information

The M31 Globular Cluster System

The M31 Globular Cluster System The M31 Globular Cluster System How alike are the GC systems of the Milky Way and M31? Jean Brodie UCO/Lick Observatory UCSC 1 GCs trace the star formation and assembly GC formation occurs early Accompanies

More information

Science Olympiad Astronomy C Division Event Golden Gate Invitational February 11, 2017

Science Olympiad Astronomy C Division Event Golden Gate Invitational February 11, 2017 Science Olympiad Astronomy C Division Event Golden Gate Invitational February 11, 2017 Team Name: Team Number: Directions: ~Answer all questions on the answer sheet provided. ~Please do NOT access the

More information

Pre-observations and models

Pre-observations and models Pre-observations and models Carine Babusiaux Observatoire de Paris - GEPI GREAT-ITN, IAC, September 2012 The questions 1) Can the observing program tackle the scientific problem? 2) What is the best configuration

More information

Gravitational waves from Massive Primordial Black Holes as Dark Matter

Gravitational waves from Massive Primordial Black Holes as Dark Matter Gravitational waves from Massive Primordial Black Holes as Dark Matter based on S. Clesse & JGB, arxiv:1603.05234 S. Clesse & JGB, Phys Rev D92 (2015) 023524 JGB, Linde & Wands, Phys Rev D54 (1996) 6040

More information

Binary sdb Stars with Massive Compact Companions

Binary sdb Stars with Massive Compact Companions Hot Subdwarf Stars and Related Objects ASP Conference Series, Vol. 392, c 2008 U. Heber, S. Jeffery, and R. Napiwotzki, eds. Binary sdb Stars with Massive Compact Companions S. Geier, 1 C. Karl, 1 H. Edelmann,

More information

Distance Measuring Techniques and The Milky Way Galaxy

Distance Measuring Techniques and The Milky Way Galaxy Distance Measuring Techniques and The Milky Way Galaxy Measuring distances to stars is one of the biggest challenges in Astronomy. If we had some standard candle, some star with a known luminosity, then

More information

Science Olympiad Astronomy C Division Event. National Cathedral School Invitational Washington, DC December 3 rd, 2016

Science Olympiad Astronomy C Division Event. National Cathedral School Invitational Washington, DC December 3 rd, 2016 Science Olympiad Astronomy C Division Event National Cathedral School Invitational Washington, DC December 3 rd, 2016 Name: Start Time: Directions: 1) Please turn in all materials at the end of the event.

More information

Astronomy: Division C Science Olympiad, Round 1 Tryout Test

Astronomy: Division C Science Olympiad, Round 1 Tryout Test Astronomy: Division C Science Olympiad, Round 1 Tryout Test Student Name : Student Number : DIRECTIONS 1. Write the answers that you want graded legibly on the answer sheet, along with your name and student

More information

THE GALAXY. Spitzer Space Telescope Images & Spectra: 3µm - 170µm

THE GALAXY. Spitzer Space Telescope Images & Spectra: 3µm - 170µm THE GALAXY Composite infrared colour image of Galactic Centre region taken at 1.25, 2.2 and 3.5 microns with COBE/DIRBE instrument (NASA/GSFC). GALAXY: A conglomeration of stars, gas + dust Topics: Star

More information

The Deaths of Stars. The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant.

The Deaths of Stars. The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant. The Deaths of Stars The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant. Once the giant phase of a mediummass star ends, it exhales its outer

More information

HD Transits HST/STIS First Transiting Exo-Planet. Exoplanet Discovery Methods. Paper Due Tue, Feb 23. (4) Transits. Transits.

HD Transits HST/STIS First Transiting Exo-Planet. Exoplanet Discovery Methods. Paper Due Tue, Feb 23. (4) Transits. Transits. Paper Due Tue, Feb 23 Exoplanet Discovery Methods (1) Direct imaging (2) Astrometry position (3) Radial velocity velocity Seager & Mallen-Ornelas 2003 ApJ 585, 1038. "A Unique Solution of Planet and Star

More information

Stellar collisions and their products

Stellar collisions and their products Stellar collisions and their products Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund University www.astro.lu.se KEY IDEA #1 Collision rate depends on V. Stellar encounter timescales

More information

Early works. Dynamics of accretion, the role of turbulence, the role of magnetic fields in the ISM, spectrum. Victorij Shvartsman

Early works. Dynamics of accretion, the role of turbulence, the role of magnetic fields in the ISM, spectrum. Victorij Shvartsman Isolated BHs Early works «Halos around black holes» Soviet Astronomy Astronom. Zhurn (1971) In this paper accretion onto isolated BHs from the ISM was studied for different BH masses (including intermediate).

More information

2019 Astronomy Team Selection Test

2019 Astronomy Team Selection Test 2019 Astronomy Team Selection Test Acton-Boxborough Regional High School Written by Antonio Frigo Do not flip over this page until instructed. Instructions You will have 45 minutes to complete this exam.

More information

The Stars. Background & History The Celestial Sphere: Fixed Stars and the Luminaries

The Stars. Background & History The Celestial Sphere: Fixed Stars and the Luminaries The Stars Background & History The Celestial Sphere: Fixed Stars and the Luminaries The Appearance of Stars on the Sky Brightness and Brightness Variations Atmospheric Effects: Twinkling Variable Stars

More information

Active Galactic Nuclei-I. The paradigm

Active Galactic Nuclei-I. The paradigm Active Galactic Nuclei-I The paradigm An accretion disk around a supermassive black hole M. Almudena Prieto, July 2007, Unv. Nacional de Bogota Centers of galaxies Centers of galaxies are the most powerful

More information

Astronomy. Stellar Evolution

Astronomy. Stellar Evolution Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am Stellar Evolution Main Sequence star changes during nuclear fusion What happens when the fuel runs out Old stars and second

More information

The Star Clusters of the Magellanic Clouds

The Star Clusters of the Magellanic Clouds The Dance of Stars MODEST-14 The Star Clusters of the Magellanic Clouds Eva K. Grebel Astronomisches Rechen-Institut Zentrum für Astronomie der Universität Heidelberg Star Clusters in the Magellanic Clouds!

More information

Neutron Star Mass Distribution in Binaries

Neutron Star Mass Distribution in Binaries A Tribute to Gerry@2013.11.26 Neutron Star Mass Distribution in Binaries Chang-Hwan Lee @ Sabbatical Year@Stony Brook (2013.8~2014.8) 1 2 Gerry s Three Questions The Future The Life The Science 3 20 years

More information

6 th lecture of Compact Object and Accretion, Master Programme at Leiden Observatory

6 th lecture of Compact Object and Accretion, Master Programme at Leiden Observatory 6 th lecture of Compact Object and Accretion, Master Programme at Leiden Observatory Accretion 1st class study material: Chapter 1 & 4, accretion power in astrophysics these slides at http://home.strw.leidenuniv.nl/~emr/coa/

More information

This Week in Astronomy

This Week in Astronomy Homework #8 Due Wednesday, April 18, 11:59PM Covers Chapters 15 and 16 Estimated time to complete: 40 minutes Read chapters, review notes before starting This Week in Astronomy Credit: NASA/JPL-Caltech

More information

ACTIVE GALACTIC NUCLEI: optical spectroscopy. From AGN classification to Black Hole mass estimation

ACTIVE GALACTIC NUCLEI: optical spectroscopy. From AGN classification to Black Hole mass estimation ACTIVE GALACTIC NUCLEI: optical spectroscopy From AGN classification to Black Hole mass estimation Second Lecture Reverberation Mapping experiments & virial BH masses estimations Estimating AGN black hole

More information

University of Naples Federico II, Academic Year Istituzioni di Astrofisica, read by prof. Massimo Capaccioli. Lecture 16

University of Naples Federico II, Academic Year Istituzioni di Astrofisica, read by prof. Massimo Capaccioli. Lecture 16 University of Naples Federico II, Academic Year 2011-2012 Istituzioni di Astrofisica, read by prof. Massimo Capaccioli Lecture 16 Stellar populations Walter Baade (1893-1960) Learning outcomes The student

More information

Dancing in the dark: spotting BHS & IMBH in GC

Dancing in the dark: spotting BHS & IMBH in GC Dancing in the dark: spotting BHS & IMBH in GC ARI-ZAH, Heidelberg University Star Clusters around the Milky Way and in the Local Group Heidelberg August 15th-17th, 2018 Unravelling stellar black hole

More information

DEPARTMENT OF PHYSICS AND ASTRONOMY. Planets around white dwarfs Matt Burleigh

DEPARTMENT OF PHYSICS AND ASTRONOMY. Planets around white dwarfs Matt Burleigh DEPARTMENT OF PHYSICS AND ASTRONOMY Planets around white dwarfs Matt Burleigh Contents Original motivation DODO - results from our direct imaging survey Where do we go next? The role for E-ELT Direct imaging

More information

HR Diagram, Star Clusters, and Stellar Evolution

HR Diagram, Star Clusters, and Stellar Evolution Ay 1 Lecture 9 M7 ESO HR Diagram, Star Clusters, and Stellar Evolution 9.1 The HR Diagram Stellar Spectral Types Temperature L T Y The Hertzsprung-Russel (HR) Diagram It is a plot of stellar luminosity

More information

Extrasolar Planets. Methods of detection Characterization Theoretical ideas Future prospects

Extrasolar Planets. Methods of detection Characterization Theoretical ideas Future prospects Extrasolar Planets Methods of detection Characterization Theoretical ideas Future prospects Methods of detection Methods of detection Methods of detection Pulsar timing Planetary motion around pulsar

More information

Observational evidence for black holes

Observational evidence for black holes Chapter 14 Observational evidence for black holes By definition an isolated black hole should be a difficult object to observe directly. However, if black holes exist they should often be accreting surrounding

More information

Massive Stellar Black Hole Binaries and Gravitational Waves

Massive Stellar Black Hole Binaries and Gravitational Waves BH-BH binaries: modeling Massive Stellar Black Hole Binaries and Gravitational Waves Chris Belczynski1 Tomek Bulik1 Daniel Holz Richard O Shaughnessy Wojciech Gladysz1 and Grzegorz Wiktorowicz1 1 Astronomical

More information

The Extragalactic Distance Scale

The Extragalactic Distance Scale One of the important relations in Astronomy. It lets us Measure the distance to distance objects. Each rung on the ladder is calibrated using lower-rung calibrations. Distance Objects Technique 1-100 AU

More information

The cosmic distance scale

The cosmic distance scale The cosmic distance scale Distance information is often crucial to understand the physics of astrophysical objects. This requires knowing the basic properties of such an object, like its size, its environment,

More information

Hubble s Law. Tully-Fisher relation. The redshift. λ λ0. Are there other ways to estimate distances? Yes.

Hubble s Law. Tully-Fisher relation. The redshift. λ λ0. Are there other ways to estimate distances? Yes. Distances to galaxies Cepheids used by Hubble, 1924 to show that spiral nebulae like M31 were further from the Sun than any part of the Milky Way, therefore galaxies in their own right. Review of Cepheids

More information

Science Olympiad Astronomy C Division Event National Exam

Science Olympiad Astronomy C Division Event National Exam Science Olympiad Astronomy C Division Event National Exam University of Nebraska-Lincoln May 15-16, 2015 Team Number: Team Name: Instructions: 1) Please turn in all materials at the end of the event. 2)

More information

OGLE-TR-56. Guillermo Torres, Maciej Konacki, Dimitar D. Sasselov and Saurabh Jha INTRODUCTION

OGLE-TR-56. Guillermo Torres, Maciej Konacki, Dimitar D. Sasselov and Saurabh Jha INTRODUCTION OGLE-TR-56 Guillermo Torres, Maciej Konacki, Dimitar D. Sasselov and Saurabh Jha Harvard-Smithsonian Center for Astrophysics Caltech, Department of Geological and Planetary Sciences University of California

More information

Gravitational Waves. Masaru Shibata U. Tokyo

Gravitational Waves. Masaru Shibata U. Tokyo Gravitational Waves Masaru Shibata U. Tokyo 1. Gravitational wave theory briefly 2. Sources of gravitational waves 2A: High frequency (f > 10 Hz) 2B: Low frequency (f < 10 Hz) (talk 2B only in the case

More information

LISA: From the Quantum to the Cosmos. Lee Samuel Finn Penn State University

LISA: From the Quantum to the Cosmos. Lee Samuel Finn Penn State University LISA: From the Quantum to the Cosmos Lee Samuel Finn Penn State University Why Gravitational Strong gravitational wave sources are compact with internal bulk motion v ~ c Energetic astronomical phenomena

More information