Gaseous debris discs around white dwarfs

Gaseous debris discs around white dwarfs Christopher J. Manser Collaborators: Boris Gänsicke, Tom Marsh, Detlev Koester, Dimitri Veras, Nicola Pietro Gentile Fusillo C.Manser@Warwick.ac.uk Saturn to scale Artists impression of SDSS J1228+14 by Mark Garlick. Image of Saturn from NASA s Cassini mission, NASA image saturn_malmercassini_5m.jpg

Talk Outline One - The gaseous debris disc around SDSS J1228+14 Few - Common variability of gaseous debris discs Many - Frequency of gaseous debris discs around white dwarfs

Remnant Planetary Systems SDSS J1228+14 Observable He atom Heavy atom HST/COS Jura & Young, 214, Annu. Rev. Earth Planet. Sci., 42, 45 JWST/MIRI Planetary debris White C and dwarf O C and O Roche limit JWST/MIRI Dust sublimation Photospheric absorption Gänsicke et. al. 212, MNRAS, 424, 333

Remnant Planetary Systems SDSS J1228+14 Observable Observable He atom Heavy atom He atom Heavy atom HST/COS HST/COS Jura & Young, 214, Annu. Rev. Earth Planet. Sci., 42, 45 Norm Flux 3. 2.5 2. 1.5 1..5 Ca ii triplet Gas JWST/MIRI 845 85 855 86 865 87 875 Roche limit Roche limit Planetary debris Planetary debris JWST/MIRI JWST/MIRI Dust sublimation Dust sublimation White C and dwarf O C and O Photospheric absorption Dust Brinkworth et. al. 29, ApJ, 696, 142 Gänsicke et. al. 212, MNRAS, 424, 333

The gaseous component of the debris disc 25 3. Ca ii triplet 2.5 Fλ [1 16 erg cm 2 s 1 Å 1 ] 2 15 1 Norm Flux 2. 1.5 1..5 845 85 855 86 865 87 875 5 SDSS J1228+14 4 5 6 7 8 9 Gänsicke et. al. 26, Science, 314, 198

Accretion disc in a binary

1 out of 18 18 23-3 23-3 21-4 21-4 16 14 26-7 26-7 211-1 211-1 12 1 8 27-7 27-7 212-3 212-3 6 28-7 28-7 214-3 214-3 4 2 29-2 29-2 215-5 215-5 85 86 87 85 86 87

Doppler Tomography Marsh & Horne, 1988, MNRAS, 235, 269

Doppler Tomography 216 12 }{{} 18 23-3 75 215-5 215-6 16 5 212-3 14 27-7 27-7 25 12 vy [km s 1 ] -25 29-4 2. R.2 R 1 8 211-1 211-4 -5 26-7 6 214-3 214-3 -75 23-3 4 75 5 25-25 -5-75 v x [km s 1 ] Manser et. al. 216, MNRAS, 455, 4467 2 215-5 215-5 85 86 87

Doppler Tomography v y [km s 1 ] 25 5 75-75 75 5 25-25 -5-75 v x [km s 1 ] -5-25 29-4 212-3 Red 211-1 26-7 215-5 215-6 216 12 }{{} 23-3 2. R.2 R Manser et. al. 216, MNRAS, 455, 4467

New observations in March and May 18 23-3 2.5 2. 216 March 16 14 27-7 27-7 1.5 1..5 12 1 8 6 4 2 211-1 211-4 214-3 214-3 215-5 215-5. 845 85 855 86 865 87 2.5 2. 1.5 1..5. 216 May 85 86 87 845 85 855 86 865 87

A Whole New Map 75 5 212-3 216 12 }{{} 22 23-3 23-3 215-5 2 18 16 27-7 27-7 vy [km s 1 ] 25-25 -5-75 29-4 26-7 23-3 2. R.2 R 75 5 25-25 -5-75 v x [km s 1 ] Manser et. al. in prep. 14 12 1 8 6 4 2 211-1 211-4 214-3 214-3 215-5 215-5 216-3 216-3 85 86 87

Some more comparing 75 215-5 216 12 }{{} 75 215-5 215-6 216 12 }{{} 5 5 25 212-3 25 212-3 vy [km s 1 ] 29-4 2. R.2 R vy [km s 1 ] 29-4 2. R.2 R -25-25 -5 26-7 -5 26-7 -75 23-3 -75 23-3 75 5 25-25 -5-75 v x [km s 1 ] Manser et. al. in prep. New (2 epochs) 75 5 25-25 -5-75 v x [km s 1 ] Old (18 epochs)

Spiral? 216 12 }{{} 75 215-5 5 25 212-3 vy [km s 1 ] 29-4 2. R.2 R -25-5 -75 26-7 23-3 75 5 25-25 -5-75 v x [km s 1 ]

Even newer data! 2.5 2. 216 May 1.5 1..5. 845 85 855 86 865 87 2.5 2. 217 March 1 1.5 1..5. 845 85 855 86 865 87

Reached half way? 3.5 3. 26 Flipped 217 2.5 2. 1.5 1..5-12 -8-4 4 8 12 Velocity [km/s]

Coadded X-Shooter spectrum 1.2 1.5 3. 2. Ca ii 8498 ; 8542; 8662 Å O i 8446 Å 1.1 1. Ca K 3934 Å CaH 3969Å 1.25 1. Mg ii 4481 Å 1..975 84 85 86 87 392 394 396 398 444 447 45 1.1 1.5 1. Fe ii 4924 Å Feii 518 Å Fe ii 5169 ; 5198 Å Feii 5235 ; 5276 ; 5317 Å Si ii 541 ; 556 Å 1.3 49 5 51 52 53 54 O i 7772 ; 7774 ; 7775 Å O i 8446 Å Mg i 886 ; O i 882 Å O i &Mgii blend 1.2 1.1 1. Mg ii 7877 ; 7896 Å O i blend Ca ii 8912 ; 8927 Å.9 775 8 825 85 875 9 925

April 21 Hubble Spectrum 1.2. 115 1155 116 125 1255 126 1265 1.2 21 1295 13 135 131 1334 1336 137 1375 138 1385 1395 14 145 141 1415 Gänsicke et. al. 212, MNRAS, 424, 333

March 216 Hubble Spectrum 1.2 115 1155 116 1.2 1295 13 135 131 1334 1336. 125 1255 126 1265 216 137 1375 138 1385 1395 14 145 141 1415 Manser et. al. in prep.

Comparing the two 1.2 115 1155 116 1.2 1295 13 135 131 1334 1336. 125 1255 126 1265 21 216 137 1375 138 1385 1395 14 145 141 1415 Manser et. al. in prep.

Circumstellar gas 1.2 115 1155 116 1.2 1295 13 135 131 1334 1336. 125 1255 126 1265 21 216 137 1375 138 1385 Si IV 1395 14 145 141 1415 Manser et. al. in prep.

Circumstellar gas 1.2 75 215-5 216 12 }{{} 5 212-3 25 115 1155 116 1.2 vy [km s 1 ] -25-5 -75 29-4 26-7 1295 13 135 131 23-3 2. R.2 R 75 5 25-25 -5-75 v x [km s 1 ] 1334 1336. 125 1255 126 1265 21 216 137 1375 138 1385 Si IV 1395 14 145 141 1415 Manser et. al. in prep.

Other variable gas discs SDSS J1228+14 22 23-3 2 18 27-7 16 14 12 1 211-1 214-3 8 6 215-5 4 2 216-3 85 86 87 Manser et. al. 216, MNRAS, 455, 4467

Morphologically variable SDSS J845+2257 SDSS J1228+14 SDSS 24 WHT 28 22 23-3 2 UVES 28 18 27-7 UVES Gemini S 29 21 16 14 12 1 211-1 214-3 X-shooter 211 8 6 215-5 X-shooter 214 4 2 216-3 85 855 86 865 Wavelength (Å) 85 86 87 Wilson et. al. 214, MNRAS, 451, 3237 Manser et. al. 216, MNRAS, 455, 4467

Morphologically variable SDSS J845+2257 SDSS J1228+14 SDSS J143+855 SDSS 24 7.5 7. 23-4 SDSS 6.5 WHT 28 22 23-3 6. UVES 28 2 5.5 27-2 WHT 18 27-7 5. UVES Gemini S X-shooter 29 21 211 16 14 12 1 8 211-1 214-3 4.5 4. 3.5 3. 2.5 29-2 WHT 21-4 WHT 211-1 X-Shooter X-shooter 214 6 4 215-5 2. 1.5 211-5 X-Shooter 85 855 86 865 Wavelength (Å) 2 85 86 87 1..5 212-1 SDSS 845 85 855 86 865 87 Wavelength (Å) Wilson et. al. 215, MNRAS, 451, 3237 Manser et. al. 216, MNRAS, 455, 4467 Manser et. al. 216, MNRAS, 462 1461 216-3

Variable strength SDSS J1617+162 Wilson et. al. 214, MNRAS, 445, 1878

Variable strength SDSS J1617+162 SDSS J1228+14 22 23-3 2 18 27-7 16 14 12 1 211-1 214-3 8 6 215-5 4 2 216-3 Wilson et. al. 214, MNRAS, 445, 1878 85 86 87 Manser et. al. 216, MNRAS, 455, 4467

Variability e - Gaseous emission Name Type ) Features a - Gaseous absorption SDSS J738+1835 SDSS J845+2257 SDSS J959 2 SDSS J143+855 WD 1144+529 SDSS J1228+14 HE 1349 235 SDSS J1617+162 DB DB DA DA DA DA DBA DA e e, v e, v e, v e e, a, v e e, v v - Spectroscopic or photometric Variability Wilson et. al. 214, MNRAS, 445, 1878

Variability 6.5 7. 23-4 SDSS 6. 27-2 WHT 5.5 SDSS 24 5. 29-2 WHT Name SDSS J738+1835 SDSS J845+2257 SDSS J959 2 SDSS J143+855 WD 1144+529 SDSS J1228+14 HE 1349 235 SDSS J1617+162 Type DB DB DA DA DA DA DBA DA ) Features e e, v e, v e, v e e, a, v e e, v 4.5 4. 3.5 3. 2.5 2. 1.5 Normalized Flux 1..5 1.3 1.2 1.1 1. 21-4 WHT 211-1 X-Shooter 211-5 X-Shooter 212-1 SDSS.9 Wavelength (Å) 845 85 855 86 865 87 Wavelength (Å) of HE 1349 235. The MagE data have been smoothed with a 5 pixel boxcar th Melis et. al. 212, ApJL, 715, L4 8 2 214-3 845 85 855 86 865 87

Detected Remnant Planetary System statistics Metal pollution Koester et. al. 214 25-5 %

Detected Remnant Planetary System statistics Metal pollution Koester et. al. 214 25-5 % Dusty disc Farihi et al. 29; Rocchetto et al. 215 1-3 %

Detected Remnant Planetary System statistics Metal pollution Koester et. al. 214 25-5 % Dusty disc Farihi et al. 29; Rocchetto et al. 215 1-3 % Gaseous component??? %

The sample Figure 2. Colour colour diagrams illustrating the location of the 27 639 DR7 spectroscopic objects that we used as training sample for our selection method. DA white dwarfs, non-da white dwarfs, NLHS and quasars are shown as blue, yellow, red and green dots, respectively. The colour cuts that define our initial broad selection from Table 2 are overlaid as red lines. Objects outside this selection were not classified and are therefore plotted as grey dots. Gentile Fusillo et. al. 215, MNRAS, 448, 226

The sample s searching for Ca ii bris disc. We also list but no observation of -.5 Exposure time [s] 45 66 45 42 27 36 3 27 36 27 18 18 18 u g u g 12-7 12-7 12-6 12-7 12-7 12-6 12-8 12-7 12-7 7-24 1-29 1-29 1-29 DA DB DAB Other..5 -.6 - SDSS J1228+14 SDSS J1617+162 SDSS J845+2257 SDSS J143+855 SDSS J738+1835 SDSS J1144+529 SDSS J959 2 - -.2..2 g g rr Figure 1. u g, g r magnitude plot of the magnitude/colour

The frequency of gaseous discs 4 35 3. 2.5 Ca ii triplet 979 single white dwarfs Fλ [1 16 erg cm 2 s 1 Å 1 ] 3 25 2 15 Norm Flux 2. 1.5 1..5 845 85 855 86 865 87 875 1 5 4 5 6 7 8 9

The frequency of gaseous discs 4 35 3. 2.5 Ca ii triplet 979 single white dwarfs Fλ [1 16 erg cm 2 s 1 Å 1 ] 3 25 2 15 Norm Flux 2. 1.5 1..5 845 85 855 86 865 87 875 1 6 Gasesous components 4 5 5 6 7 8 9

Detected Remnant Planetary System statistics Metal pollution Koester et. al. 214 25-5 % Dusty disc Farihi et al. 29; Rocchetto et al. 215 1-3 % Gaseous component.7 %

Detected Remnant Planetary System statistics Metal pollution Koester et. al. 214 25-5 % Dusty disc Farihi et al. 29; Rocchetto et al. 215 1-3 % Gaseous component.7 % Debris discs with a gaseous component 2-1 %

Summary SDSS J1228+14 is well studied, but still many unanswered questions. An observable gaseous component appears to be linked with variability Determined the frequency of a gaseous component to a debris disc at a white dwarf.