Distances to galaxies - INAF-OAC · 2011. 6. 17. · Extragalactic stellar astronomy . The...

Distances to galaxies from

the brightest stars in the universe

Rolf Kudritzki

in collaboration with

Miguel UrbanejaFabio Bresolin

Vivian UZachGazak

requires independent accurate methods to

assess systematic effects

δH0 / H0 < 5%

Extragalactic stellar astronomy The perennial problem of extragalactic distances

patchy dust extinction

metallicity

dependenceof distance indicators

metal-poor

metal-rich

HII regions in M83HII regions in M83

4000Å 6000Å

Pagel, Edmunds, Blackwell et al. 1979

strong line method: R23 = f[N(O)/N(H)]

simple empirical calibration

but…

depends on

Telectronnelectronnature of

ionizing stars

gas imhomog.

filling factors

depletion into

dust…..

Extragalactic stellar astronomy ΛCDM-universe

metallicity

of galaxies depends on their mass

metal-rich

metal-poor

metal-medium

NGC 300M81

Extragalactic stellar astronomy Tremonti

et al., 2004, ApJ

613, 898

50,000 starforming

galaxies with Sloan spectra

strong nebularemission lines:hydrogen,oxygen,nitrogen

Extragalactic stellar astronomy mass-metallicity

relationship

Rosetta stoneto understandgalaxy formationand chemical evolution!

However…It’s based on very simplified emission line analysis….

Tremonti

et al., 2004, ApJ

613, 898

Extragalactic stellar astronomy SDSS star forming galaxies

Kewley & Ellison 2008

mass –

metallicityrelationship

depends crucially on strong line method

calibration

supergiant stars will come to rescue !!!!

Extragalactic stellar astronomy the alternative –

quantitative spectroscopy of the brightest stars

Fabio Bresolin

2011 supergiants

objects in transition

B1–A4

Brightest normal stars

at visual light:

105..106

Lsun-7 ≥

-10 mag

yrsL, M ~ const.

ideal to determine

• chemical compos.• abundance grad.• SF history• extinction• extinction laws• distances

of galaxies

nearby supergiants

in Orion

1000 Lyrs

2011 Flux weighted Gravity –

Luminosity Relationship (FGLR)

Kudritzki, Bresolin, Przybilla, ApJ

Letters, 582, L83 (2003)

M ~ g×R2

~ L×(g/T4) = const.

const.

with L ~ Mx

~ Lx(g/T4)x, x ~ 3

~ (g/T4)x

or with Mbol

~ -2.5log L

= a log(g/T4) + b FGLR

a =2.5 x/(1-x) ~ 3.75

L,M ~ const.

Example: LMC FGLR using Magellan/Mage

Urbaneja, Kudritzki, Pietrzynski, Gieren

et al., 2011

LMC BSG RV

and E(B-V)

= 0.12 mag

Urbaneja, Kudritzki, Pietrzynski, Gieren

et al., 2011

2011 Spectroscopic studies

beyond the Local Group

• selection of targets from wide field CMDs

• HST ACS imaging

• multi-object spectroscopy∆λ

~ 4-5 A with FORS @ VLT

LRIS @ Keck

~ 4%, ∆

log g ~ 0.05, metallicity

~ 0.1 dex

• galaxies out to 10 Mpc

011 pilot study

NGC 300NGC 300 – Sculptor Group (2 Mpc)

117 cepheids

70 blue supergiant spectra

Kudritzki, Urbaneja, Bresolin

et al. 2008, ApJ

681, 269

The power of modern spectroscopy

Galactic template

NGC 300 A2 supergiant

A grid of NLTE model calculations

Late-B (B6) to mid-A (A3/A5)•

Luminosity class: Ia

to Ib/II•

12 metallicities

Z/Z_sun•

2.0, 1.4, 1.0, 0.7, 0.5, 0.4, 0.3, 0.25, 0.2, 0.14, 0.1, 0.05

Chemical composition•

H,He,C,N,O,Mg,S,Ti,Fe•

Ne,Na,Al,Si,P,K,Ca,Sc,V,Cr,

Mn,Co,Ni,Cr,Zn,Sr,Y,Zr,Ba

~ 6000 models in total

14,000 10,000Teff

Balmer

jump fitting: Teff

= 9500K

bf-absorptionby hydrogenfrom 2nd

= 9250K

Balmer

jump fitting: Teff

= 9750K

Balmer

jump fitting: Teff

= 9500K

Balmer

jump fitting: Teff

Balmer

series fitting: log g = 1.55±0.1

At fixed Teff

log g = ±

Balmer

series fitting: log g = 1.55±0.1

At fixed Teff

log g = ±

A2 IaTeff

= 9500 Klog g = 1.45

HST/ACS + ground

Kudritzki, Urbaneja

& Bresolin

et al. 2008

SED fit E(B-V), RVAVextinction law

NGC 300A supergiant

E(B-V) distribution in NGC 300

Adopted byHST Key ProjectFreedman et al.2001

Distance 15%too large

NGC 300 (log g, log Teff

diagram

40 25 15 Msun

B supergiants(Urbanejaet al., 2005) A supergiants

(Kudritzki et al., 2008)

011 Kudritzki, Urbaneja, Bresolin

et al, 2008, ApJ

681, 269

regression

= 3.41{ log(g/T4eff,4

) -1.5} –

8.02 = 0.32 mag

Kudritzki, Urbaneja, Bresolin

et al., 2008, ApJ

681, 269

Study of metallicities

Metallicity: spectral window

[Z] = -1.3 …

Spectral window 4497-4607Å

χ2i =SN

2 1npix

npixj=1 (Oj − Cj)2

spectral window 4497-4607Å

another spectral window

all windows

[Z] = -0.4±0.1

A3 IaTeff = 8500Klog g = 1.65

all windows

[Z] = -0.5±0.15

Stellar metallicity

gradient in NGC300

B0 –

B3 supergiants●

B8 –

A4 supergiants---

log{Z/Z_sun} = -0.03 –

0.45•ρ/ρ0

= -0.03 –

0.08•d/kpc

Kudritzki, Urbaneja, Bresolin, Przybilla, Gieren, Pietrzynski, 2008, ApJ

681, 269angular galactocentric

distanceρ0

= 9.75 arcmin

5.7kpc

“Extragalactic Pizza” IfA March 1st 2005 53 - 40

Extragalactic Stellar Spectroscopy

Stellar vs. HII Stellar vs. HII metallicitymetallicity

gradient gradient

Zaritsky

et al. (1994) ----

Dopita

&Evans (1986) ----

Kobolnicky

et al. (1999) ----

Denicolo

et al. (2002)

Almost identical with stellar regression!!!!

Pilyugin

(2001) ----

Pettini

& Pagel

(2004) Who is right???

Kudritzki

et al., 2008, ApJ

681, 265

auroral

nebular lines

The solution? Auroral

lines!!

28 auroral line detections(previously: 2)

VLT/FORS2NGC 300

Bresolin, Gieren, Kudritzki, Pietrzynsky, Urbaneja & Carraro 2009, ApJ, 700,

Bresolin,Gieren, Kudritzki

et al. 2009

Excellent agreement between auroral

lines and supergiants

◦ ●

auroral□

* supergiants

HII-auroral

lines regression

supergiants

regression

this work

McGaugh91Tremonti

et al.2004

Kewley/Dopita2002

Pettini/Pagel2004

Auroral

lines vs. strong lines calibrations –

a horror story !!

Bresolin,Gieren, Kudritzki

et al. 2009

NGC 300

0.6 dex

Bresolin, Gieren, Kudritzki, Pietrzynsky, Urbaneja & Carraro

2009, ApJ, 700, 309

WLMWLMfaintest dwarf irregular in LGfew HII regions: [O] = -0.8

A-supergiant: [Fe] = -1.00Urbaneja, Kudritzki, Bresolin

et al. 2008, ApJ, 684, 118

average of 6

A-supergiants: [Fe] = -0.87±0.07

2011 FGLR in WLM

FGLR distance d= 0.99 ±0.05

Urbaneja, Kudritzki, Bresolin

et al.2008

ApJ, 684, 118

agrees with Cepheids, TRGB Pietrzynski

et al., 2008,

et al., 2007

2011An FGLR distance to M33

from A & B supergiants

Vivian U, Miguel Urbaneja, Rolf Kudritzki et al., 2009, ApJ

740, 1120

Published distances to M33method m-M (mag) authors

Cepheids 24.52 ± 0.14 Lee et al., 2002

24.62 ± 0.15 Freedman et al., 200125.53 ± 0.11 Scowcroft et al., 2009

TRGB 24.81 ± 0.15 Kim et al., 200224.69 ± 0.15 Tiede

et al., 2004

24.50 ± 0.15 McConnachie

et al., 2004 24.64 ± 0.15 Gallet

et al., 2004

HB 24.84 ± 0.16 Sarajedini

et al., 2000PNLF 24.86 ± 0.11 Ciardullo

et al., 2004

RR Lyrae 24.67 ± 0.16 Sarajedini

et al., 2000

24.85 ± 0.13 Pierce et al., 2000H2

O masers 24.31 ± 0.45 Brunthaler

et al., 2005Binary 24.92 ± 0.12

Bonanos, Stanek, Kudritzki

et al., 2006

2011 A supergiants

in M33

Vivian U, Urbaneja, Kudritzki, Jacobs, Bresolin, 2009, ApJ

740, 1120

B&A supergiants

in M33

740, 1120

B&A supergiants

in M33 -

reddening

740, 1120

011 B&A supergiants

in M33 –

Vivian U, Urbaneja, Kudritzki et al. 2009

m-M = 24.93±0.11 mag

B&A supergiants

in M33

B supergiants• A

740, 1120

shallow slope 0.07 dex/kpc

011 Cepheids

in M33

Scowcroft et al, 2009, MNRAS 396, 1287

Magrini

et al., 2007 metallicity

gradient

U, Urbaneja, Kudritzki

et al. 2009

Bresolin

M81 Keck LRIS

2011 M81 extinction

Distance too large

the extinction problem

for ∆E(B-V) = 0.2

@ H-band ∆Aλ

= 0.12 mag∆d/d

= 5.5%

M81 FGLR

M81●

other galaxies

m-M = 27.62 ±

0.09 mag

Kudritzki, Gazak, Urbaneja

et al.

very shallow gradient: 0.02 dex/kpc

super solar [Z]

NGC2403 3.5 MpcKeck LRISData taken January 2011

NGC 4258 7 Mpc

“Maser Galaxy”

Keck LRIS March 26 –

28, 2011

Bresolin, 2011auroral

Zaritsky

et al., 1994strong lines

Metallicity

of NGC 4258

McGaugh, 1991strong lines

2011Cepheids

in NGC 4258

HII regions

et al. 2006, Riess

et al., 2009

using Zaritsky

et al., 1994

Bresolin

2011 Blue supergiants

in NGC 4258

Keck LRIS March 26 –

28, 2011

011 NGC 4258, Mask 1, Slit 5

= 8300K, log g = 0.75[Z] = -0.2

Thirty Meter Telescope (TMT)

TMT on Mauna Kea

WFOS quantitative spectroscopy possible down to mV

~ 24.5 mag

with objects MV

- 8 mag

M ~ 32.5 mag

~ 30 Mpc

possible

chemical evolution studiesSFISM, extinction, extinction lawsdistances

10 objects per galaxy

Δ(m-M) ~ 0.1 mag

Conclusions and TMT/ELT perspectives

Gaia first accurate distances of MW BSGsMW BSG too far for Hipparcos

accurate calibration of FGLRso far: average of 8 galaxies

LMC calibration under way

Conclusions and Gaia perspectives

Distances to galaxies - INAF-OAC · 2011. 6. 17. · Extragalactic stellar astronomy . The...

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