Glenn van de Ven Institute for Advanced Study

Slides:



Advertisements
Similar presentations
To measure the brightness distribution of galaxies, we must determine the surface brightness of the resolved galaxy. Surface brightness = magnitude within.
Advertisements

Effects of galaxy formation on dark matter haloes Susana Pedrosa Patricia Tissera, Cecilia Scannapieco Chile 2010.
Padova 03 3D Spectrography 3D Spectrography IV – The search for supermassive black holes.
Analysis of a New Gravitational Lens FLS Yoon Chan Taak Feb Survey Science Group Workshop
Slide 1 Andromeda galaxy M31Milky Way galaxy similar to M31.
Current Observational Constraints on Dark Energy Chicago, December 2001 Wendy Freedman Carnegie Observatories, Pasadena CA.
Clusters & Super Clusters Large Scale Structure Chapter 22.
H.-W. Rix, Vatican 2003 Gravitational Lensing as a Tool in Cosmology A Brief History of Lensing 1704 Newton (in Optics): „Do not bodies act upon light.
PRESENTATION TOPIC  DARK MATTER &DARK ENERGY.  We know about only normal matter which is only 5% of the composition of universe and the rest is  DARK.
Dark Matter in Galaxies using Einstein Rings Brendon J. Brewer School of Physics, The University of Sydney Supervisor: A/Prof Geraint F. Lewis.
Physics 133: Extragalactic Astronomy and Cosmology Lecture 12; February
Physics 133: Extragalactic Astronomy and Cosmology Lecture 13; February
First Results from an HST/ACS Snapshot Survey of Intermediate Redshift, Intermediate X-ray Luminosity Clusters of Galaxies: Early Type Galaxies and Weak.
On the Distribution of Dark Matter in Clusters of Galaxies David J Sand Chandra Fellows Symposium 2005.
CDM cusps in LSB galaxies by means of stellar kinematics A.Pizzella, E.M.Corsini, F. Bertola Università di Padova And J. Magorrian, M. Sarzi University.
Constraining Galactic Halos with the SZ-effect
Lens Galaxy Environments Neal Dalal (IAS), Casey R. Watson (Ohio State) astro-ph/ Who cares? 2.What to do 3.Results 4.Problems! 5.The future.
Galaxy-Galaxy Lensing What did we learn? What can we learn? Henk Hoekstra.
Survey Science Group Workshop 박명구, 한두환 ( 경북대 )
Galaxy Characteristics Surface Brightness Alternative to Luminosity I(R) = Flux/area = erg/s/cm 2 /arcsec 2 I(0) – center flux I(R) = at radius R Define.
Effects of baryons on the structure of massive galaxies and clusters Oleg Gnedin University of Michigan Collisionless N-body simulations predict a nearly.
Application of Gravitational Lensing Models to the Brightest Strongly Lensed Lyman Break Galaxy – the 8 o’clock arc E. Buckley-Geer 1, S. Allam 1,2, H.
Eric V. Linder (arXiv: v1). Contents I. Introduction II. Measuring time delay distances III. Optimizing Spectroscopic followup IV. Influence.
Cosmic shear results from CFHTLS Henk Hoekstra Ludo van Waerbeke Catherine Heymans Mike Hudson Laura Parker Yannick Mellier Liping Fu Elisabetta Semboloni.
Complementarity of weak lensing with other probes Lindsay King, Institute of Astronomy, Cambridge University UK.
Intrinsic ellipticity correlation of luminous red galaxies and misalignment with their host dark matter halos The 8 th Sino – German workshop Teppei O.
PREDRAG JOVANOVIĆ AND LUKA Č. POPOVIĆ ASTRONOMICAL OBSERVATORY BELGRADE, SERBIA Gravitational Lensing Statistics and Cosmology.
PNe as mass tracers Dark-to-luminous properties of early-type galaxies Nicola R. Napolitano Kapteyn Institute Groningen (NL) ESO workshop: PNe beyond the.
The masses and shapes of dark matter halos from galaxy- galaxy lensing in the CFHTLS Henk Hoekstra Mike Hudson Ludo van Waerbeke Yannick Mellier Laura.
Gravitational Lensing Analysis of CLASH clusters Adi HD 10/2011.
Γαλαξίες – 3 Υπερμαζικές Μαύρες Τρύπες στα κέντρα γαλαξιών 15 Ιανουαρίου 2013.
Constraining Cosmography with Cluster Lenses Jean-Paul Kneib Laboratoire d’Astrophysique de Marseille.
Modeling the dependence of galaxy clustering on stellar mass and SEDs Lan Wang Collaborators: Guinevere Kauffmann (MPA) Cheng Li (MPA/SHAO, USTC) Gabriella.
Racah Institute of physics, Hebrew University (Jerusalem, Israel)
Correlations of Mass Distributions between Dark Matter and Visible Matter Yuriy Mishchenko and Chueng-Ryong Ji NC State University Raleigh, NC KIAS-APCTP-DMRC.
Cosmic shear and intrinsic alignments Rachel Mandelbaum April 2, 2007 Collaborators: Christopher Hirata (IAS), Mustapha Ishak (UT Dallas), Uros Seljak.
April 3, 2005 The lens redshift distribution – Constraints on galaxy mass evolution Eran Ofek, Hans-Walter Rix, Dan Maoz (2003)
Strong Lensing Surveys and Statistics Dan Maoz. zqzq Survey strategies: Search among source population for lensed cases or Search behind potential lenses.
Subaru Wide-Field Survey of M87 Globular Cluster Populations N.Arimoto (NAOJ) N.Tamura, R.Sharples (Durham) M.Onodera (Tokyo, NAOJ), K.Ohta(Kyoto) J.-C.Cuillandre.
How Different was the Universe at z=1? Centre de Physique Théorique, Marseille Université de Provence Christian Marinoni.
Gravitational Lensing
KASI Galaxy Evolution Journal Club A Massive Protocluster of Galaxies at a Redshift of z ~ P. L. Capak et al. 2011, Nature, in press (arXive: )
Competitive Science with the WHT for Nearby Unresolved Galaxies Reynier Peletier Kapteyn Astronomical Institute Groningen.
Mass Profiles of Galaxy Clusters Drew Newman Newman et al. 2009, “The Distribution of Dark Matter Over Three Decades in Radius in the Lensing Cluster Abell.
What Shapes Galaxies?STScI, 27 April 2016 Anne-Marie Weijmans University of St Andrews Tim de Zeeuw, Eric Emsellem, Davor Krajnović, Pierre-Yves Lablanche.
Chapter 20 Cosmology. Hubble Ultra Deep Field Galaxies and Cosmology A galaxy’s age, its distance, and the age of the universe are all closely related.
The prolate shape of the Galactic halo Amina Helmi Kapteyn Astronomical Institute.
Constraining Dark Energy with Double Source Plane Strong Lenses Thomas Collett With: Matt Auger, Vasily Belokurov, Phil Marshall and Alex Hall ArXiv:
Bayesian analysis of joint strong gravitational lensing and dynamic galactic mass in SLACS: evidence of line-of-sight contamination Antonio C. C. Guimarães.
Cosmology with Strong Lensing.
The Origin and Structure of Elliptical Galaxies
Thomas Collett Institute of Astronomy, Cambridge
Thomas Collett Institute of Astronomy, Cambridge
Cosmology with gravitational lensing
Dynamical Models for Galaxies Observed with SAURON Michele Cappellari
Thomas Collett Institute of Astronomy, Cambridge
Cosmological Constraints from the Double-
Advisors: Tom Broadhurst, Yoel Rephaeli
Dynamical constraints on the mass of the black hole in a ULX
Mapping the Universe With radio galaxies and quasars.
Globular Clusters with Gemini
Galactic Astronomy 銀河物理学特論 I Lecture 1-4: Dynamical structures of galaxies Seminar: Cappellari et al. 2006, MNRAS, 366, 1126 Lecture: 2011/10/24.
The SAURON Survey - The stellar populations of early-type galaxies
UVIS Calibration Update
Niranjan Sambhus, Flavio De Lorenzi, Ortwin Gerhard (Basel)
Intrinsic Alignment of Galaxies and Weak Lensing Cluster Surveys Zuhui Fan Dept. of Astronomy, Peking University.
Yongmin Yoon, Myungshin Im, Gwang-ho Lee, Gu Lim, and Seong-kook Lee
THE X-RAY C-M RELATION FABIO GASTALDELLO INAF-IASF MILANO, UCI
Photometric Properties of Spiral Galaxies
Presentation transcript:

Glenn van de Ven Institute for Advanced Study glenn@ias.edu Probing dark matter in galaxies with gravitational lensing and kinematics Glenn van de Ven Institute for Advanced Study glenn@ias.edu

Cold dark matter simulations …galaxies are embedded in extended dark matter distributions with a close to universal profile and triaxial shape Almost all observations based on collecting light… Need conversion from dark matter to (luminous) baryons: ‘adding’ baryons using empirical prescriptions ‘subtracting’ baryons from total mass distribution inferred through luminous tracers of the gravitational potential a b c (b/a)dm ~ 0.7 (c/a)dm ~ 0.5 (Jing & Suto 2002) The now-standard cold DM cosmological model predicts that … Since almost all observations are based on collecting light, we can test these predictions only by converting between dark and luminous baryonic matter. This conversion can be done in two ways… The main goal of my proposal is to use this second approach to constrain both the profile and shape of the DM distribution. HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Photometric observations M51 = NGC 5194 NGC 4365 If we then look for these luminous tracers, its is obvious that the spiral galaxies have a very complex appearance with lost of obscuring dust. On the other hand, elliptical galaxies appear very simple with mainly stars as clean luminous tracers. Late-type galaxies: complex with lots of obscuring dust Early-type galaxies: simple with (mainly) stars as clean tracers HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Integral-field spectroscopy To measure the kinematics of the stars we can use integral-field spectroscopy. An array of lenslets provides at every position on the plane of the sky a spectrum, from which we can extract, for example, the kinematics of the stars. … a spectrum at every position on the plane of the sky HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Stellar kinematic observations NGC 4660 [-150/+150 km/s] NGC 4365 [-58/+58 km/s] z x z triaxial oblate axisymmetric HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Stellar dynamical models Most early-type galaxies consistent with oblate axisymmetry SAURON paper IX: Emsellem et al. (2007,MNRAS,379,401) SAURON paper X: Cappellari et al. (2007,MNRAS,379,418) SAURON paper XII: Krajnovič et al. (2008,MNRAS,390,93) Triaxial dynamical models of giant ellipticals… van de Ven, de Zeeuw & van den Bosch (2008,MNRAS,385,614) van den Bosch, van de Ven, et al. (2008,MNRAS,385,647) van den Bosch & van de Ven (2008,MNRAS,arXiv:0811.3474) …still dominated by short-axis tube orbits “Simple” axisymmetric models at high(er) redshift? HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Stellar kinematics at higher-z In a very recent project, I used another integral-field spectrograph, GMOS at the GEMINI south telescope, to obtain kinematics of the inner parts of a galaxy at a distance about 10 times as far as our typical kinematic observations so far. Although quite challenging we were able to extract a very nice velocity and dispersion field. From fitting a dynamical model we find an M/L… Applying stellar population models to the spectra and images at different wavelengths we estimate a stellar M/L… This provides with at most 20% DM in the inner parts. Perhaps even more important is that this proofs the feasibility of detailed stellar dynamical modeling at increasing redshift. GMOS spectrograph ~4 hours on-source z=0.04 (D=155 Mpc) van de Ven et al. (2008,ApJ,arXiv:0807.4175) HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Axisymmeric dynamical model Mass-anisotropy degeneracy: radial variation in l.o.s. velocity dispersion due to change in mass or velocity anisotropy Total mass-to-light ratio: M/L=3.7±0.5 M/L HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Strong gravitational lensing zl=0.0394 (D=155 Mpc) zs=1.695 However, as you have noticed, this is a rather special galaxy, since it also acts as a lens galaxy that deflects the light of a distant quasar into four images in a cross-like configuration: well-known as the Einstein Cross Since GL is sensitive to the total mass, the images provide alternative luminous tracers. Below, on the left, is again the observed LIGHT distribution (with HST), and on the right is the TOTAL MASS distribution as obtained by fitting a lens model to the positions and fluxes of the four quasar images. This yields also a M/L that is consistent with the dynamical one, and again, at most a 20% DM fraction. This is a crucial test of both kinematics and GL as luminous tracers. The strong advantage of GL over kinematics is that it “only” requires (good) imaging. In particular, the upcoming deep and wide imaging surveys like … are expected to reveal a vast number of these lensing events, allowing constraints on the DM distribution at high redshift. The Einstein Cross QSO 2237+0305 HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Strong gravitational lens model source position flux ratio Mass-sheet degeneracy: additional mass along line-of-sight Scale-free projected potential (Evans & Witt, 2003,MNRAS,345,1351) Predict image positions and flux ratios: 2x4+3 = 11 constraints Slope , quasar position (ξ,η) + 7 Fourier coeff. = 10 parameters HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

surface brightness = light Surface density surface brightness = light … “mass follows light” in projected shape lens model = mass RE~1” HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Mass distribution projected mass Projected flat ME/LE=3.4 M/L round lens models ME/LE=3.4 M/L luminous density round density ellipticity flat Rein Re round Intrinsic HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies" circular velocity

Dark matter fraction Dynamical mass-to-light ratio: 3.7 ± 0.5 M/L Mass and light within Einstein radius: 3.4 ± 0.1 M/L Stellar mass-to-light ratio: HST central V, I, R, H and K colors SSP models with Kroupa IMF, 0.01–120 M (Vazdekis et al. 2006) …best-fit t=8 Gyr and [Fe/H]=0.2: M*/L = 3.3 M/L …range t=7–14 Gyr and [Fe/H]=0.0–0.3: M*/L=2.8 – 4.1 M/L Inner R<4” ~ 2/3 Re bulge-dominated region of ~L* lens galaxy: mass follows light, at most ~20% constant dark matter fraction HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Isothermal conspiracy? Total mass density isothermal? (e.g., Koopmans et al. 2006) Strong lensing provides constraints only around Einstein radius! Einstein Cross: projected Galaxy models: projected slope lens models luminous density lens models luminous density dark matter isothermal isothermal stars van de Ven, Mandelbaum & Keeton (2008,MNRAS,arXiv:0808.2493) HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Isothermal conspiracy? Total mass density isothermal? (e.g., Koopmans et al. 2006) Strong lensing provides constraints only around Einstein radius! Einstein Cross: projected Galaxy models: deflection curve lens models luminous density isothermal isothermal dark matter stars van de Ven, Mandelbaum & Keeton (2008,MNRAS,arXiv:0808.2493) HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Lensing cross section σ(x) Selection biases strong lens galaxies all galaxies + magnification bias Lensing cross section σ(x) HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Orientation and shape Total cross section: higher long-axis along l.o.s. Four-image: higher intermediate axis along l.o.s. Three-image: only for very flat projections, but possibly misclassified quads Total: no shape bias if averaged over viewing angles 4/2-ratio: probe of shape, but dependence on e.g. source luminosity function total 4/2-ratio projected flattening HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Dark matter inner slope total 4/2-ratio Strong selection bias with dark matter inner slope (> adiabatic contraction) Total: independent of shape and magnification bias 4/2-ratio: weak dependence shape + magnification bias Degenerate with concentration… DM inner slope HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Dark matter concentration Total cross section total 4/2-ratio DM concentration DM inner slope HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Lensing and kinematics Lensing in photometric surveys, and kinematics at increasing redshift: constraints on dark matter distribution …but first understand selection and modeling biases Simulation pipeline for lensing and kinematics by galaxy models (van de Ven, Mandelbaum & Keeton, 2008,MNRAS,arXiv:0808.2493) Selection biases in strong lensing surveys (Mandelbaum, van de Ven & Keeton, 2008,MNRAS,arXiv:0808.2497) Strong lensing modeling biases (Keeton, Mandelbaum & van de Ven, in prep.) Stellar kinematics modeling biases (cf. van de Ven, de Zeeuw & van den Bosch 2008,MNRAS,385,614) Strong lensing and stellar kinematics biases HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Summary in figures HFS, March 10, 2009 Einstein Cross NGC 4365 NGC 3379 HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

END HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Isothermal conspiracy? Total mass density isothermal? (e.g., Koopmans et al. 2006) Strong lensing provides constraints only around Einstein radius! Galaxy models (stars + DM) van de Ven, Mandelbaum & Keeton (2008,MNRAS,arXiv:0808.2493) HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Image separation: spherical Singular isothermal sphere (SIS): Δθ=2Rein Distributions highly skewed towards SIS Consistent with “isothermal conspiracy” Nearly independent of DM inner slope or magnification bias DM inner slope HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Image separation: non-spherical Long-axis in plane highest mean image separation Intermediate axis along l.o.s. highest width image sep. distribution edge-on face-on side-on end-on l.o.s.=long-axis l.o.s.=intermediate-axis l.o.s.=short-axis DM inner slope HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Sersic: cross section vs. index Lower mass Higher mass dm dm stars stars HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"

Sersic: Einstein radius total stars dark matter Einstein radius HFS, March 10, 2009 Glenn van de Ven, "Probing dark matter in galaxies"