Probing the ISM at z > 3 with rest-frame UV emission from LAEs - - PowerPoint PPT Presentation

Probing the ISM at z > 3 with rest-frame UV emission from LAEs in MUSE-Wide

Kasper B. Schmidt

Leibniz-Institut für Astrophysik Potsdam (AIP) & The MUSE Collaboration:

• K. B. Schmidt, kbschmidt@aip.de

Sakura CLAW, Tokyo, March 26 2018

• Demographics:
• Clustering in (R.A., Dec., z), number counts (LF),
• But also physics of the systems:
• Stellar mass
• Star formation rate
• Electron density
• Temperature
• Gas phase metallicity
• Kinematics and velocities
• etc.
• Main probes are rest-frame optical photometry and spectroscopy
• But at z > 3 observed optical corresponds to rest-frame UV

Main Goal: Understanding Galaxies

2

• K. B. Schmidt, kbschmidt@aip.de

Sakura CLAW, Tokyo, March 26 2018

Probing ISM/Galaxy prop. with UV lines

3

• Have to rely on rest-frame UV for early Universe studies: Lyα, CIII, CIV
• Lyα gives redshift, SFR(?) and relates to Hydrogen column density
• CIII], CIV, HeII, [OIII]4363, etc probe:
• ionizing radiation (logU), gas-phase metallicity (Z), electron density (ne)

Rigby+15 Super solar Sub solar

(Until JWST is launched)

• K. B. Schmidt, kbschmidt@aip.de

Sakura CLAW, Tokyo, March 26 2018

Probing ISM/Galaxy prop. with UV lines

3

• Have to rely on rest-frame UV for early Universe studies: Lyα, CIII, CIV
• Lyα gives redshift, SFR(?) and relates to Hydrogen column density
• CIII], CIV, HeII, [OIII]4363, etc probe:
• ionizing radiation (logU), gas-phase metallicity (Z), electron density (ne)

Rigby+15 Super solar Sub solar

(Until JWST is launched)

Gutkin+16

• K. B. Schmidt, kbschmidt@aip.de

Sakura CLAW, Tokyo, March 26 2018

Probing ISM/Galaxy prop. with UV lines

3

• Have to rely on rest-frame UV for early Universe studies: Lyα, CIII, CIV
• Lyα gives redshift, SFR(?) and relates to Hydrogen column density
• CIII], CIV, HeII, [OIII]4363, etc probe:
• ionizing radiation (logU), gas-phase metallicity (Z), electron density (ne)

Rigby+15 Super solar Sub solar

(Until JWST is launched)

Gutkin+16 Maseda+17

• K. B. Schmidt, kbschmidt@aip.de

Sakura CLAW, Tokyo, March 26 2018

• MUSE GTO program; PI: Lutz Wisotzki
• 100 ⨉ 1arcmin2 MUSE pointing mosaic on CDF-S and COSMOS
• 1 hour exposures reaching 6σ point-source EL depth ≲10-17erg/s/cm2
• Main Science Goals:

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Bright Lyα Emitters

Complete census of z > 3 LAEs (exploiting multi-λ HST data) Physical properties of LAEs Studying extreme EW objects LAE Luminosity Functions Describe Lyα halos and Blobs

Spectra of Everything!

Immense legacy value for the broader community Discovery potential

Low & Intermediate z Galaxies:

Spatially Resolved Spectroscopy + HST Low mass galaxies (≳ 107M ) Studying Faint AGN

• R. Saust’s poster

• K. B. Schmidt, kbschmidt@aip.de

Sakura CLAW, Tokyo, March 26 2018

Emission Line Sources in MW

5 3.0 3.5 4.0 4.5 5.0 5.5 6.0 6.5 7.0 redshift 10 20 30 40 50

Lyα

674 LAEs from first 60 MUSE-Wide pointings

Lyα [OII] Balmer break absorption Hβ + [OIII] Hα + SII 6.53 0.04

z

The first 60 fields

• K. B. Schmidt, kbschmidt@aip.de

Sakura CLAW, Tokyo, March 26 2018

Emission Line Sources in MW

5 3.0 3.5 4.0 4.5 5.0 5.5 6.0 6.5 7.0 redshift 10 20 30 40 50

Lyα

674 LAEs from first 60 MUSE-Wide pointings

Lyα [OII] Balmer break absorption Hβ + [OIII] Hα + SII 6.53 0.04

z

The first 60 fields

However, As of last week, this has been added the sources from 40 more fields… Details are on

• T. Urrutia’s Poster

• K. B. Schmidt, kbschmidt@aip.de

Sakura CLAW, Tokyo, March 26 2018

• Despite MUSE sensitivity at 1hr detection is still challenging
• Initial comparison in overlap with deep fields confirm this
• Optimal extraction of spectra to improve S/N with:
• Multi-component GALFIT model of HST counterpart
• Representation of models in full 3D MUSE cube
• Simultaneous extraction of all sources in FoV
• Full 3D per-pixel representation of each source
• Collapsed 1D spectra with optimal S/N

UV lines in MUSE-Wide LAEs

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https://github.com/ kasperschmidt/TDOSE

• K. B. Schmidt, kbschmidt@aip.de

Sakura CLAW, Tokyo, March 26 2018

• Searching for CIII and CIV doublets in MUSE-Wide LAEs
• MUSE covers CIII] at 2.9 < z < 3.9 & CIV at 2.9 < z < 5.0 for LAEs

UV lines in MUSE-Wide LAEs

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50 100 150 200 EW( Lyα ) / [ ˚ A] 10 20 30 40 50 60 70 80 EW( CIII]λ1909 ˚ A ) / [ ˚ A] 0.0 0.8 1.6 2.4 3.2 4.0 4.8 5.6 6.4 7.2 8.0 redshift 50 100 150 200 EW( Lyα ) / [ ˚ A] 10 20 30 40 50 60 70 80 EW( CIVλ1548 ˚ A ) / [ ˚ A] 0.0 0.8 1.6 2.4 3.2 4.0 4.8 5.6 6.4 7.2 8.0 redshift 80 8.0 12

1:1 relation 1:3 relation 1:10 relation Bayliss et al. (2014) Erb et al. (2010) Hoag et al. in press. Huang et al. (2016) Rigby et al. (2014) Rigby et al. (2015), IUE Rigby et al. (2015), MagE Rigby et al. (2015), STIS Schmidt et al. (2017) Shapley et al. (2003) Stark et al. (2014) Stark et al. (2015b) Stark et al. (2016) Vanzella et al. (2016) Vanzella et al. (2017)

8.0

Mainali et al. (2017) Smit et al. (2017)

• K. B. Schmidt, kbschmidt@aip.de

Sakura CLAW, Tokyo, March 26 2018

• Searching for CIII and CIV doublets in MUSE-Wide LAEs
• MUSE covers CIII] at 2.9 < z < 3.9 & CIV at 2.9 < z < 5.0 for LAEs

UV lines in MUSE-Wide LAEs

7

50 100 150 200 EW( Lyα ) / [ ˚ A] 10 20 30 40 50 60 70 80 EW( CIII]λ1909 ˚ A ) / [ ˚ A] 0.0 0.8 1.6 2.4 3.2 4.0 4.8 5.6 6.4 7.2 8.0 redshift 50 100 150 200 EW( Lyα ) / [ ˚ A] 10 20 30 40 50 60 70 80 EW( CIVλ1548 ˚ A ) / [ ˚ A] 0.0 0.8 1.6 2.4 3.2 4.0 4.8 5.6 6.4 7.2 8.0 redshift 80 8.0 12

1:1 relation 1:3 relation 1:10 relation Bayliss et al. (2014) Erb et al. (2010) Hoag et al. in press. Huang et al. (2016) Rigby et al. (2014) Rigby et al. (2015), IUE Rigby et al. (2015), MagE Rigby et al. (2015), STIS Schmidt et al. (2017) Shapley et al. (2003) Stark et al. (2014) Stark et al. (2015b) Stark et al. (2016) Vanzella et al. (2016) Vanzella et al. (2017)

8.0

Mainali et al. (2017) Smit et al. (2017)

50 100 150 200 EW( Lyα ) / [ ˚ A] 10 20 30 40 50 60 70 80 EW( CIII]λ1909 ˚ A ) / [ ˚ A] 0.0 0.8 1.6 2.4 3.2 4.0 4.8 5.6 6.4 7.2 8.0 redshift 50 100 150 200 EW( Lyα ) / [ ˚ A] 10 20 30 40 50 60 70 80 EW( CIVλ1548 ˚ A ) / [ ˚ A] 0.0 0.8 1.6 2.4 3.2 4.0 4.8 5.6 6.4 7.2 8.0 redshift

See also Maseda+17 & in prep. work in MUSE deep fields

• K. B. Schmidt, kbschmidt@aip.de

Sakura CLAW, Tokyo, March 26 2018

UV lines in MUSE-Wide LAEs

8

• Searching for CIII and CIV doublets in MUSE-Wide LAEs
• MUSE covers CIII] at 2.9 < z < 3.9 & CIV at 2.9 < z < 5.0 for LAEs
• Initial guess on zsys from Verhamme et al. (submitted)
• First step: Obtain EW estimates from potential line detections
• Forced flux estimate on optimally extracted spectra
• Template matching around zsys for UV lines/doublets independently
• First tests recover lines well in mock spectra
• Extend to larger template grid, and apply to MUSE-Wide LAEs

1895 1900 1905 1910 1915 1920 Wavelength [A] −2 2 Flux

Mock spectrum CIII-doublet template CCmax location

• K. B. Schmidt, kbschmidt@aip.de

Sakura CLAW, Tokyo, March 26 2018

Acknowledgements

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P.I. R. Bacon* P.I. L. Wisotzki*

• C. Diener
• C. Herenz
• J. Kerutt*
• R. Saust*
• K. Schmidt*
• T. Urrutia*

*At Sakura CLAW