High redshift dwarf galaxies with ELT/MOSAIC Arjan Bik (Stockholm - - PowerPoint PPT Presentation

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High redshift dwarf galaxies with ELT/MOSAIC Arjan Bik (Stockholm - - PowerPoint PPT Presentation

Jan 17, 2023 331 likes •558 views

High redshift dwarf galaxies with ELT/MOSAIC Arjan Bik (Stockholm University) Gran stlin (SU), Emil Rivera-Thorsen (Oslo), Veronica Menacho (SU) Dwarf Galaxies -CDM cosmology: Hierarchical model of galaxy formation: Small

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SLIDE 1

High redshift dwarf galaxies with ELT/MOSAIC

Arjan Bik

(Stockholm University)

Göran Östlin (SU), Emil Rivera-Thorsen (Oslo), Veronica Menacho (SU)

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SLIDE 2

Dwarf Galaxies

  • Λ-CDM cosmology: Hierarchical model of galaxy

formation:

  • Small structures formed and merge to larger

galaxies (White & Rees 1978).

  • Many more dwarf galaxies in the early universe.

Steepening of the galaxy luminosity function at high z (e.g. Mortlock et al. 2015).

  • Candidates for re-ionization of the universe

(Bouwens et al, 2016).

  • At high redshift: mostly star forming
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SLIDE 3

Blue Compact (Dwarf) Galaxies

  • Use local analogues of high-redshift dwarf galaxies.
  • Strongly star forming, dozens of super star clusters
  • within a few 100 Mpc

Optical Lya, UV, Ha UV, optical, Ha

  • HST Lya imaging & BB imaging, COS UV spectroscopy

(LARS: Östlin et al, 2014, Hayes et al, 2014)

  • VLT/MUSE integral field spectroscopy
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SLIDE 4

Blue Compact Galaxies

DISTANCE (MPC) MASS

(Msun)

12+LOG(O/H) SFR (MSUN/YR) HARO 11 88

9x109 stars 5.1x108 HI 8.1-8.3 22.0

ESO 338 37.5

4x109 stars 1.4x109 HI 7.9 3.2

SBS 0335 54

7X107 stars 4.2X108 HI 7.3 1.3

References: Östlin et al, 1998, Östlin et al, 2001, Bergvall & Östlin 2002, Cannon et al, 2004, Guseva et al, 2012, Adamo et al, 2010; Bergvall 2006, Pardy et al, 2016, Guseva et al, 2012, Ekta et al, 2009

ESO 338-IG04 Haro 11 SBS-0335-052E

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SLIDE 5

Blue Compact Galaxies

DISTANCE (MPC) MASS

(Msun)

12+LOG(O/H) SFR (MSUN/YR) HARO 11 88

9x109 stars 5.1x108 HI 8.1-8.3 22.0

ESO 338 37.5

4x109 stars 1.4x109 HI 7.9 3.2

SBS 0335 54

7X107 stars 4.2X108 HI 7.3 1.3

References: Östlin et al, 1998, Östlin et al, 2001, Bergvall & Östlin 2002, Cannon et al, 2004, Guseva et al, 2012, Adamo et al, 2010; Bergvall 2006, Pardy et al, 2016, Guseva et al, 2012, Ekta et al, 2009

ESO 338-IG04 Haro 11 SBS-0335-052E

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SLIDE 6

MUSE @z~0

  • Spatially resolved kinematics: galaxy scale outflow
  • No ordered rotation: outflows, mergers ect…

ESO 338-IG04 SBS-0335-052E

Bik et al, 2015 Herenz et al, 2017

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SLIDE 7

MUSE @z~0

  • Ionisation mapping [OIII]/Halpha:
  • Ionisation cones where LyC is likely to escape
  • Halos are density bound, LyC could leak out

ESO338 Haro 11

Menacho et al, submitted Bik et al, 2018

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SLIDE 8
  • HDM mode: small IFUs with a spatial sampling of 0.08”/

pixel, R=5000 of selected galaxies

  • HMM mode: integrated spectra of many faint, high z dwarf

galaxies

  • We expect 1 Haro 11 type galaxy per 0.1 z bin in a MOSAIC

FOV.

  • Many more lower mass galaxies: ideal for MOSAIC
  • Websim/COMPASS (Puech et al., 2016) simulations to

predict observables with ELT/MOSAIC

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SLIDE 9
  • Can we spatially resolve the

halos of high-z BCDs?

  • Kinematics
  • Ionization parameter
  • abundances
  • Further and deeper: integrated

light with the HMM

  • MUSE data as input
  • 0.45 - 1.8 micron:
  • Halpha until z=1.7
  • [OIII] until z=2.4
  • Lya from z=3
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SLIDE 10

Haro 11 with MOSAIC in 10h

z=0.5 z=1.0 z=1.5 [OIII], z=2.0 [OIII], z=2.4

1“=6.3 kpc 1“=8.7 kpc 1“=8.6 kpc 1“=8.3 kpc 1“=7.9 kpc 1“=0.4 kpc

Halpha, z=0

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SLIDE 11

ESO 338 & SBS0335

Halpha, z=1.0 [OIII], z=2.4

1“=8.7 kpc 1“=7.9 kpc 1“=0.2 kpc

Halpha, z=0

1“=8.7 kpc 1“=8.6 kpc 1“=0.03 kpc

Halpha, z=1.0 Halpha, z=1.5

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SLIDE 12

Kinematics

Halpha, z=0.5 Halpha, z=0.02

Haro 11

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SLIDE 13

Kinematics

v_Halpha, z=0.5 v_Halpha, z=1.5 v_Halpha, z=0

  • Spatially resolved kinematics: galaxy scale outflow
  • No ordered rotation: outflows, mergers ect…
  • At high z: not that clear! Large structures will be visible.

ESO 338-IG04

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SLIDE 14

Ionisation mapping

OIII/Halpha, z=0.02 OIII/Hbeta, z=1.0 Haro 11

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SLIDE 15

Ionisation mapping

OIII/Halpha, z=0.02 OIII/Hbeta, z=1.0 PSF matching!!

  • OIII/SII (Pelligrini et al, 2012)

Haro 11

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SLIDE 16

Abundances

Einy, Bik et al, in prep

ESO 338-IG04

  • With MUSE we can make 2D metallicity and N/O ratio

maps —> trace assembly history, feedback by massive stars.

  • ELT/MOSAIC will enable this at high redshift.

N/O 12+log(O/H)

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SLIDE 17

Integrated light with HMM

  • High-multiplex mode: reach fainter galaxies (lower

masses)

  • Metallicities (mass-metallicity relation)
  • global ionization, HeII, OIII/OII
  • rest frame UV stellar absorption features: what are

the massive star properties at z=3 and beyond?

  • neutral ISM absorption lines.
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SLIDE 18

Integrated light with HMM

  • High-multiplex mode: reach fainter galaxies (lower

masses)

  • Metallicities (mass-metallicity relation)
  • global ionization, HeII, OIII/OII
  • rest frame UV stellar absorption features: what are

the massive star properties at z=3 and beyond?

  • neutral ISM absorption lines.

Wofford et al, 2011

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SLIDE 19

Integrated light with HMM

  • High-multiplex mode: reach fainter galaxies (lower

masses)

  • Metallicities (mass-metallicity relation)
  • global ionization, HeII, OIII/OII
  • rest frame UV stellar absorption features: what are

the massive star properties at z=3 and beyond?

  • neutral ISM absorption lines.

Wofford et al, 2011

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SLIDE 20

Summary

  • The HDM mode of MOSAIC enables spatially resolved

studies of low-mass starbursts to z ~ 2.

  • Spatially resolved kinematics: study in detail galaxy

scale outflows.

  • Ionisation mapping: what is f_esc of LyC photons at

z=1-2? (does it increase?)

  • Make spatially resolved abundance maps
  • HMM mode: fainter galaxies, absorption lines