The MUSE Quasar-field Blind Emitter Surveys (MUSEQuBES)

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1 The MUSE Quasar-field Blind Emitter Surveys (MUSEQuBES) Sowgat Muzahid Leiden Observatory The Netherlands June 12, 2018 S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

2 MUSEQuBES MUSEQuBES COLLABORATION: Sean Johnson, Sowgat Muzahid, Joop Schaye (PI), Marijke Segers, Lorrie Straka, Martin Wendt + MUSE consortium OUTLINE: Very Brief Overview of MUSE Survey Designs and Preliminary Results MUSEQuBES-I (CGM of low-z Galaxies; z < 1.0) MUSEQuBES-II (CGM of high-z Lyα emitters; z > 2.9) S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

3 Brief Overview of MUSE Integral-field spectrograph (Imager + Spectrograph) on VLT/UT4 FoV: 1 1 (WFM); (NFM) 24 sub-fields, each is fed into an integral-field unit (IFU) Spatial sampling: = contains 90,000 spectra! Spectral coverage: Å; R 3000 Adaptive optics system GALACSI has been commissioned recently 255 nights of GTO time! S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

4 MUSE-QuBES Surveys MUSE-QuBES I (Low-z ) 16 QSO fields (Depths: 2 10 hrs) 65 hrs of MUSE GTO observations Hα: [O iii]: [O ii]: HST/COS spectra of QSOs z qso: R 20,000; S/N per res. element Targeted absorption lines: H i, O vi, Si iii, C iii, N v 300 galaxies are detected (z < z qso) (continuum selected; SExtractor) 50 galaxies (pure line emitter) The largest uniform sample (with ρ <300 kpc)! Ancillary Data: HST/ACS (for all): Gal. morphology, kinematics VLT/UVES (for some): Abs. kinematics IMACS, LDSS3 (for some): More galaxies S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

5 MUSE-QuBES I: An Example HE , z qso = 0.451; z gal = , ρ = 102 kpc Data: VLT/MUSE and HST/ACS S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

6 MUSE-QuBES I: An Example HE z qso = z gal = ρ = 102 kpc Data: VLT/UVES and HST/COS S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

7 MUSE-QuBES I: The Galaxy Sample Total: 318 galaxies (all continuum selected; pure line emitters are not used!) ρ kpc (Median ρ 150 kpc) Median ρ/r vir 1.78 S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

8 MUSE-QuBES I: The Galaxy Sample M : SED fitting (FAST; Kriek+09) M M vir (Moster+13) R vir (R 200 ) SFR: = Hα (Kennicutt 98) = [O ii] (Kewley+04) Median Properties: Median M = M ( Predominantly Low Mass! ) Median M vir = M Median R vir = 86 kpc Median SFR = 0.2 M yr 1 ( Mild SFR! ) Median ssfr = yr 1 ( Predominantly SFing! ) Median L = 0.1 L ( Predominantly sub-l! ) S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

9 MUSE-QuBES I: Preliminary Results Straka+ (in prep.) C f (< R vir ) = 0.43 ± 0.11 C f (< 2R vir ) = 0.32 ± 0.05 S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

10 MUSE-QuBES I: Preliminary Results Spectral Stacking (Segers+ in prep.) LOS Hubble distance [pmpc] OVI z em > 0.38 All galaxies 0.5 OVI z em > 0.38 v LOS < 100 km/s Median log 10 τovi 1.0 Det. lim. Median log 10 τovi LOS velocity [km/s] Characteristic velocity 200 km s d trans /R vir O vi is widespread out to 2R vir S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

11 MUSE-QuBES I: Preliminary Results Dependence on SFR S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

12 MUSE-QuBES I: Preliminary Results S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

13 MUSE-QuBES I: Preliminary Results Dependence on M S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

14 MUSE-QuBES I: Preliminary Results S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

15 MUSE-QuBES I: Preliminary Results Dependence on ssfr S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

16 This page is intentionally left blank! S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

17 MUSE-QuBES II MUSE-QuBES II (High-z ) 8 MUSE fields (Depths: 2 10 hrs) 51 hrs of MUSE GTO observations 8 VLT/UVES quasar spectra R 45,000 & S/N per pixel! Targeted absorption lines: H i, C iv, Si iv, N v z qso: Lyα forest is (still) not too severe! z Lyα : λ Lyα : Å free from sky lines! λ C iv : Å not severely affected by sky lines S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

18 MUSE-QuBES II: An Example v = 125 km/s v = 125 km/s z_lae = LAE ID= NB, ID= VLT/UVES QB , z = VLT/MUSE x LAE v = 230 km/s v = 230 km/s z_lae = ID= NB, ID=75 ρ=204 kpc ρ=170 kpc S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

19 MUSE-QuBES II: The Emitter Sample 75 LAEs are detected (z < z qso; Muzahid+ in prep.) (pure line emitters; CubEx [Cantalupo, in prep.]) First-ever systematic survey of the CGM of Lyα emitters The largest sample for studying the CGM of high-z galaxies (with ρ < 300 kpc) Impact Parameter (kpc) Redshift S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

20 MUSE-QuBES II: The Emitter Sample S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

21 MUSE-QuBES II: Preliminary Results Normalised Mean Flux Velocity (km/s) Low mass, continuum-faint Lyα emitters show an offset of 200 km s 1 w.r.t the z sys! An alternate means to calibrate LAE redshift (statistically)! We proposed (will propose) for KMOS (JWST) time for rest-frame optical nebular lines S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22

22 T H A N K S! S. Muzahid (Leiden Observatory) Bubbles Big & Small, Bangalore June 12, / 22 Summary We have two unique (so far the largest!) samples to study the CGM in both galaxy-centric and absorption-centric approaches MUSEQuBES-I Covering fraction of O vi around low-z SFing galaxies: 45% ( 30%) within R vir (2R vir ) The velocity over which O vi signal is detected along the LOS: 200 km s 1 ( v circ ) O vi absorption shows a positive correlation with SFR, which is actually driven by M O vi signal is significantly different for galaxies with M > M and < M O vi signal is significantly different for galaxies with ssfr > /yr and < /yr MUSEQuBES-II The LAEs in our sample show an average velocity offset of 200 km s 1