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:

Main Goal: Understanding Galaxies • 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 K. B. Schmidt, kbschmidt@aip.de Sakura CLAW, Tokyo, March 26 2018 2

Probing ISM/Galaxy prop. with UV lines • Have to rely on rest-frame UV for early Universe studies: Ly α , CIII, CIV (Until JWST is launched) • Ly α 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 (n e ) Rigby+15 Super solar Sub solar K. B. Schmidt, kbschmidt@aip.de Sakura CLAW, Tokyo, March 26 2018 3

Probing ISM/Galaxy prop. with UV lines • Have to rely on rest-frame UV for early Universe studies: Ly α , CIII, CIV (Until JWST is launched) • Ly α 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 (n e ) Gutkin+16 Rigby+15 Super solar Sub solar K. B. Schmidt, kbschmidt@aip.de Sakura CLAW, Tokyo, March 26 2018 3

Probing ISM/Galaxy prop. with UV lines • Have to rely on rest-frame UV for early Universe studies: Ly α , CIII, CIV (Until JWST is launched) • Ly α 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 (n e ) Gutkin+16 Maseda+17 Rigby+15 Super solar Sub solar K. B. Schmidt, kbschmidt@aip.de Sakura CLAW, Tokyo, March 26 2018 3

• MUSE GTO program; PI: Lutz Wisotzki • 100 ⨉ 1arcmin 2 MUSE pointing mosaic on CDF-S and COSMOS • 1 hour exposures reaching 6 σ point-source EL depth ≲ 10 -17 erg/s/cm 2 • Main Science Goals: Low & Intermediate Bright Ly α Emitters Spectra of z Galaxies: Everything! Complete census of z > 3 LAEs (exploiting multi- λ HST data) Spatially Resolved Immense legacy value for the Spectroscopy + HST broader community Physical properties of LAEs � Low mass galaxies ( ≳ 10 7 M ) Discovery potential Studying extreme EW objects Studying Faint AGN LAE Luminosity Functions Describe Ly α halos and Blobs R. Saust’s poster K. B. Schmidt, kbschmidt@aip.de Sakura CLAW, Tokyo, March 26 2018 4

Emission Line Sources in MW z 6.53 The first 60 fields Ly α [OII] Balmer break absorption H β + [OIII] H α + SII 0.04 50 Ly α 674 LAEs from first 60 40 MUSE-Wide pointings 30 20 10 0 3 . 0 3 . 5 4 . 0 4 . 5 5 . 0 5 . 5 6 . 0 6 . 5 7 . 0 redshift K. B. Schmidt, kbschmidt@aip.de Sakura CLAW, Tokyo, March 26 2018 5

Emission Line Sources in MW z 6.53 The first 60 fields Ly α [OII] However, As of last week, this has been added the sources from 40 more fields … Balmer break absorption H β + [OIII] Details are on H α + SII 0.04 50 T. Urrutia’s Poster Ly α 674 LAEs from first 60 40 MUSE-Wide pointings 30 20 10 0 3 . 0 3 . 5 4 . 0 4 . 5 5 . 0 5 . 5 6 . 0 6 . 5 7 . 0 redshift K. B. Schmidt, kbschmidt@aip.de Sakura CLAW, Tokyo, March 26 2018 5

UV lines in MUSE-Wide LAEs • 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 https://github.com/ kasperschmidt/TDOSE K. B. Schmidt, kbschmidt@aip.de Sakura CLAW, Tokyo, March 26 2018 6

UV lines in MUSE-Wide LAEs • 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 1:1 relation Erb et al. (2010) Rigby et al. (2015), IUE Shapley et al. (2003) Stark et al. (2016) 1:3 relation Hoag et al. in press. Rigby et al. (2015), MagE Stark et al. (2014) Vanzella et al. (2016) 1:10 relation Huang et al. (2016) Rigby et al. (2015), STIS Stark et al. (2015b) Vanzella et al. (2017) Smit et al. (2017) Bayliss et al. (2014) Rigby et al. (2014) Schmidt et al. (2017) Mainali et al. (2017) 80 8 . 0 12 8 . 0 80 8 . 0 80 8 . 0 7 . 2 7 . 2 70 70 6 . 4 6 . 4 60 60 A] A] A ) / [ ˚ 5 . 6 5 . 6 A ) / [ ˚ 50 50 4 . 8 4 . 8 EW( CIII] λ 1909 ˚ EW( CIV λ 1548 ˚ redshift redshift 40 40 4 . 0 4 . 0 30 30 3 . 2 3 . 2 2 . 4 2 . 4 20 20 1 . 6 1 . 6 10 10 0 . 8 0 . 8 0 0 0 . 0 0 . 0 0 50 100 150 200 0 50 100 150 200 EW( Ly α ) / [ ˚ EW( Ly α ) / [ ˚ A] A] K. B. Schmidt, kbschmidt@aip.de Sakura CLAW, Tokyo, March 26 2018 7

UV lines in MUSE-Wide LAEs • 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 1:1 relation Erb et al. (2010) Rigby et al. (2015), IUE Shapley et al. (2003) Stark et al. (2016) 1:3 relation Hoag et al. in press. Rigby et al. (2015), MagE Stark et al. (2014) Vanzella et al. (2016) 1:10 relation Huang et al. (2016) Rigby et al. (2015), STIS Stark et al. (2015b) Vanzella et al. (2017) Smit et al. (2017) Bayliss et al. (2014) Rigby et al. (2014) Schmidt et al. (2017) Mainali et al. (2017) 80 8 . 0 12 8 . 0 80 8 . 0 80 8 . 0 80 8 . 0 80 8 . 0 7 . 2 7 . 2 7 . 2 7 . 2 70 70 70 70 6 . 4 6 . 4 6 . 4 6 . 4 60 60 60 60 A] A] A] A] A ) / [ ˚ A ) / [ ˚ 5 . 6 5 . 6 5 . 6 5 . 6 A ) / [ ˚ A ) / [ ˚ 50 50 50 50 4 . 8 4 . 8 4 . 8 4 . 8 EW( CIII] λ 1909 ˚ EW( CIII] λ 1909 ˚ EW( CIV λ 1548 ˚ EW( CIV λ 1548 ˚ redshift redshift redshift redshift 40 40 40 40 4 . 0 4 . 0 4 . 0 4 . 0 30 30 30 30 3 . 2 3 . 2 3 . 2 3 . 2 2 . 4 2 . 4 2 . 4 2 . 4 20 20 20 20 1 . 6 1 . 6 1 . 6 1 . 6 10 10 10 10 0 . 8 0 . 8 0 . 8 0 . 8 0 0 0 0 0 . 0 0 . 0 0 . 0 0 . 0 0 50 100 150 200 0 50 100 150 200 0 50 100 150 200 0 50 100 150 200 EW( Ly α ) / [ ˚ EW( Ly α ) / [ ˚ EW( Ly α ) / [ ˚ EW( Ly α ) / [ ˚ A] A] A] A] See also Maseda+17 & in prep. work in MUSE deep fields K. B. Schmidt, kbschmidt@aip.de Sakura CLAW, Tokyo, March 26 2018 7

UV lines in MUSE-Wide LAEs • 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 z sys from Verhamme et al. (submitted) • First step: Obtain EW estimates from potential line detections - Forced flux estimate on optimally extracted spectra • Template matching around z sys for UV lines/doublets independently - First tests recover lines well in mock spectra - Extend to larger template grid, and apply to MUSE-Wide LAEs Mock spectrum CIII-doublet template CC max location 2 Flux 0 − 2 1895 1900 1905 1910 1915 1920 Wavelength [A] K. B. Schmidt, kbschmidt@aip.de Sakura CLAW, Tokyo, March 26 2018 8

Acknowledgements P.I. R. Bacon* P.I. L. Wisotzki* C. Diener C. Herenz J. Kerutt* R. Saust* K. Schmidt* T. Urrutia* *At Sakura CLAW K. B. Schmidt, kbschmidt@aip.de Sakura CLAW, Tokyo, March 26 2018 9