Polarimetric Survey of Giant Ly Nebulae
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1 Polarimetric Survey of Giant Ly Nebulae Yujin Yang Korea Astronomy & Space Science Institute (KASI) Chang You, Ann Zabludoff, Paul Smith, Buell Jannuzi (Steward), Moire Prescott (New Mexico), Eunchong Kim (KASI, Seoul Nat'l)
2 Giant Ly Nebulae: Key Questions Resonant scattering Polarization map (Hayes+11) Superwind (Galactic wind in M82) Radio galaxy, AGN (Reuland+03) Cold accretion/stream (Goerdt+10) What powers Ly halo? Energy source? Star formation? (SMGs; Geach+05) Resonant scattering? (Steidel+11, Hayes+11) Shock from superwind driven by stars/sne/agn? (Taniguchi+00, Wilman+05) Photo-ionization by AGNs? (Geach+09) Cold accretion/streams? (Nilsson+06, Smith+07, Rosdahl & Blaizot+11) Gas kinematics? Inflow vs outflow? Mild outflows (Yang+11,14ab) How Ly blobs will evolve into the present day? Environment? See Bădescu's poster on Ly blob's environments See Prescott and Cai's talks
3 High-redshift Ly Nebulae (Ly Blobs) Ly gas (IGM) z=3.1 galaxy? or photo-ionization by stars & AGN (H II region in M33) resonant scattering (scattering by dust in Egg Nebula) 25 ~ 200kpc Steidel blob 1 (Matsuda+04; Subaru) Discovered by narrow-band imaging (Steidel et al. 2000) at z=2 6 Direct 2D image of inter- or circum-galactic medium (IGM/CGM) Witnessing the formation of massive galaxies in groups, clusters No evidence for inflow. Only mild outflows. (Yang et al. 2011, 2014ab) Powering mechanism: photo-ionization vs. resonant scattering?
4 Where Ly Photons are Produced? resonant scattering (Hayes, Scarlata et al.) Photo-ionization: in-situ production of Ly no Ly line polarization signal Scattering: production of Ly within a central source and scattering by neutral hydrogen concentric Ly line polarization angle. P increases outwards (R. Bower 2010) Theory: Lee & Ahn (1998), Dijkstra & Loeb (2008), Trebitsch, Verhamme+2016, Chang+2017 Obs: Prescott et al. (2011), Hayes et al. (2011), Humphrey et al. (2013), Beck et al. (2016)
5 MMT/SPOL Polarization Survey Goals: Census of polarization patterns in different physical conditions. Test polarization models in various systems. Infer physical conditions of extended gas (CGM). Targets: surface-brightness limited sample: > 2e-17 cgs/sq. arcsec (1e44 erg/s) B3 J , 4C41.17: radio galaxies (z=3.087, 3.79) LABd05: obscured AGN with photoionization cone? (z=2.656) SSA22-Sb3-LAB1: radio-loud QSO (z=3.1) FLS-LAB: cold-mode accretion powered Ly halo (Smith+07)? No AGN signature. Observations: MMT/SPOL runs in , 11 nights awarded (thru. UA and KASI time) FOV = 20'' at MMT-6.5m (51'' at Bok-2.3m) Calibrated against polarized- and unpolarized-standards: instrumental polarization < 0.1% (photon-noise dominated), Peff = 97%
6 Polarimetry Basics: Stokes Parameters Stokes Left Circular Right Circular Linear Horizontal Linear Vertical Linear +45 Linear -45 Unpolarized I Q U V
7 MMT/SPOL Imaging Polarimetry (I+Q) (I Q) MMT/SPOL: dual-beam polarimeter for Stokes (I, Q, U, V) Rotate the /2-waveplate by 0, 90, 180, 270 Q+ image 45, 135, 225, 315 Q- image Q & I 22.5, 112.5, 202.5, U+ image 67.5, 157.5, 247.5, U- image U & I
8 B3 J Goal: Map polarizations in a nebula with dominant AGN photo-ionization. Target: Radio galaxy B3 J at z=3.087 Ly halo over ~130 kpc (De Breuck+03) L(Ly ) = erg/s Observation: MMT/SPOL exposure for 9.3 hours (Matsuda+09)
9 Stokes Images SB = Reduced Stokes Images (I, Q, U) First Ly imaging polarimetry of high-z radio galaxies! (You et al. 2017) You et al. (2017) ApJ, 834, 182
10 Stokes Images Smoothed with 1.2''-diameter circular tophat You et al. (2017) ApJ, 834, 182
11 Stokes Images ±3σ Chi images for Q and U You et al. (2017) ApJ, 834, 182
12 Mapping the Polarization in B3 J Radio knots (De Breuck+03) VLA 8.4GHz image Perez-Torres & De Breuck (2005) You et al. (2017) ApJ, 834, 182
13 Mapping the Polarization in B3 J Measurement apertures You et al. (2017) ApJ, 834, 182
14 Mapping the Polarization in B3 J significant detections (>2σ) You et al. (2017) ApJ, 834, 182
15 Mapping the Polarization in B3 J Detection of polarization: 5% (at 5kpc) 17% (at 30kpc) Polarization angle perpendicular to the jet direction Polarization mostly along the jet (major axis of nebula) Weak polarization along minor axis You et al. (2017) ApJ, 834, 182
16 Strong Polarization along the Jet Increasing outward Perpendicular to [aperture center] Cylindrical pattern (cf. concentric rings in Hayes+11) ionization and optical depth vary due to jet or jet-igm interaction? obscuration by AGN torus? common in HzRG? P total (8'') = 1.7% ± 0.9% < 11.9% ± 2% (LAB1) Consistent with the scattering of Ly from the central source (AGN). Scattering also plays a role in radio-galaxies with photo-ionization. You et al. (2017) ApJ, 834, 182
17 Polarization from Ly Line vs. Continuum? (Matsuda+09) same SB Could the observed polarization P(line+cont) arise from the underlying UV continuum? Unlikely. You et al. (2017) ApJ, 834, 182
18 LABd05: AGN photo-ionization powered? z=2.6 Ly Dey+05 HST, Ly image: Prescott+08,11 (Yang+14a) First detection of molecular gas in (radio-quiet) Ly blobs! CO and dust concentrated on one galaxy, an obscured AGN So far, no source found at the peak of Ly (Dey+05, Prescott+12, Yang+14a) First targeted with Ly imaging polarimetry by Prescott et al. (2011) null detection with P = 2.6% ± 2.8% AGN photo-ionization powers Ly?
19 No offset between Ly and CO toward AGN Yang et al. (2014a) AGN/CO LRIS spec. (Dey+05) Compare Ly and CO line profiles along the sight-line toward AGN Symmetric Ly profile around AGN & no velocity offset no significant inflow/outflow or static toward AGN Optically thin: photo-ionization by obscured AGN important?
20 Summary & Outlook B3 J2330 LABd05 SSA22-LAB1 Cylindrical (P=1.9%) Concentric (P=12%) (Hayes, Scarlata et al. 2011) First Ly imaging polarimetry for HzRGs (You et al. 2017). Diverse polarization patterns. Different P total = 1.9% 12%. Significant P(~20%) & scatterings are common, and varying over the nebulae. Need imaging polarimetry to guide any follow-up spectro-polarimetry. Detailed polarization modeling. Spectro-polarimetry. MMT/SPOL upgrade for blue coverage and wider FOV. Stay tuned for more polarization measurements!
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