erosita - StarsWG Jan Robrade erosita meeting, Bamberg, Oct Hamburger Sternwarte
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1 erosita - StarsWG Jan Robrade Hamburger Sternwarte erosita meeting, Bamberg, Oct. 2015
2 erosita - calibration update Eff. Area (cm 2 ) Eff. Area (cm 2 ) erosita eff. area - new vs. old (FOV/survey) 5x200Al/200PI + 2x100Al/200PI erosita_iv_7telfov_ff Energy (kev) Energy (kev) new ARFs/RMF released in May 2015, instruments multiple configurations possible, use standard survey setup Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
3 erosita - performance update normalized counts s 1 kev Energy (kev) 1 erosita spectrum of Procyon, old (red) vs. new (black) ARF+RMF 10 % less photons for softer sources Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
4 erosita - performance update F X erg cm 2 s 1 erosita spectra of Procyon and TW Hya ( 3 cts s 1 ), FOV/survey setup, 5ks good performance at relevant energies abundances and temperature structure Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
5 erosita - performance update normalized counts s 1 kev F X 0.5/ erg cm 2 s Energy (kev) erosita spectra of Capella and Lam And (5 10 cts s 1 ), FOV/survey setup, 5ks good performance at relevant energies eff. area effects for typical stellar all-sky-population quite moderate Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
6 erosita - all-sky survey and stellar content erass sensitivity with two Suns (adapted from Wright et al. 2010) The X-ray HRD (Güdel 2004) erosita survey: L Xmin d 2 (pc) erg s 1 erosita (black line) vs. ROSAT: survey+pointings (dots) Chandra: CDF-N, ChaMP, COSMOS (crosses) Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
7 erosita and stars Besancon model: (RASS, Guillout+ 1996) 0.7 million X-ray stars > 50 per deg 2 (disk), 6 per deg 2 (poles) lim. F X erg cm 2 s 1 (logs = -1.9 [cts/s], 20 cts/1600s detection limit: L X d 2 (pc) [erg/s] log N (1/deg^2) erosita X-ray stars (all, kev) Stellar surface densities at var. galactic lat./lon log S (cts/s) Simulations are based on the Besancon Stellar X-ray population model. Image by J. Robrade. ns00000 ns00090 ns00180 ns05000 ns05180 ns10000 ns10180 ns20000 ns20180 ns30000 ns30180 ns50000 ns50180 ns70000 ns70180 ns age x 6 star groups (0.15/1.0/10 Gyr, A to late M), standard coronal sources strong overall contribution from young stars ( ) young stars dominate disk (3/4 and 2/3 up to b = 0/5 deg, τ 150 Myr) Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
8 Detecting nearby young stars with erosita Nearby young stars - erass X-ray horizon 28.0 HR 8799 TW Hya --> 1kpc EK Dra, AB Dor --> 1kpc AT Mic --> 500 pc π 1 UMa--> 300 pc AD Leo --> 200 pc log Lx (erg s 1 ) late A/VLM F - mid M stars Gould Belt SFRs ( 140 pc) Pleiades (130 pc) AB Dor Tuc/Hor β Pic TWA η Cha Distance (pc) Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
9 Detecting nearby young stars with erosita Nearby young stars - erass X-ray horizon Sensitivity at 100 pc (MS): early F (5 L ) log L X /L bol = -6.3 mid M (0.005 L ) log L X /L bol = -3.3 log Lx (erg s 1 ) 28.0 HR late A/VLM F - mid M stars TW Hya --> 1kpc EK Dra, AB Dor --> 1kpc AT Mic --> 500 pc π 1 UMa--> 300 pc AD Leo --> 200 pc Gould Belt SFRs ( 140 pc) Pleiades (130 pc) AB Dor Tuc/Hor β Pic TWA η Cha Distance (pc) young+nearby (100 pc, 200 Myr) virtually all F to mid M stars closer X-ray horizon for late A and VLM stars (M7+) very nearby - RECONS 10 pc: > 300 stars ( , A-F-G-K-M) many moderately older groups in range (UMa cluster, 300 Myr; Hyades, 600 Myr...) Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
10 SFRs & T Tauri stars CTTS - WTTS - post TTS - ZAMS few old CTTS in nearby TWA, ηcha many SFRs at pc (Gould belt), strong X-ray emission in all YSOs CTTS: accretors, rare in 100pc, WTTS: weak/no accretion or disks post TTs/ZAMS - more dispersed full sky coverage ideal X (pc) Col 121 Ori OB1b Ori OB1c 10 km s 1 Per Ori Ori OB1a Cas Per OB2 Cep OB2 Tau Vela OB2 Cep α Per 0 Vela Sun Cep OB6 Tr 10 LCC Lac OB1 200 UCL Oph US GC Aqu Y (pc) Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
11 Intermediate mass stars HAeBe stars young, diverse X-ray picture coronae, jets, MCWS, companions often X-ray bright, well below saturation strong soft + hard X-ray emission repeatedly detected ApBp stars Stelzer et al. (2009) MS, diverse X-ray picture MCWS, magnetic disk, companions below & above wind line (log L X /L bol 7) strong soft + hard X-ray emission repeatedly detected Robrade & Schmitt (2011/updated) Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
12 Ultracool dwarfs UCDs - VLMs & Brown dwarfs young BD - quite hot & luminous up to log L X erg/s, mostly massive/hottest BDs typically in SFR X-ray bright UCD population in solar vicinity (20 30 pc) strong flares quite frequent Williams et al. (2014) Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
13 erosita early science - erass1 Stellar science with erass1 sample size stars census of stellar content new sources (already better than RASS) hard/absorbed sources, e.g. SFRs more comprehensive opt./ir data available + upcoming new IDs, better characterization (e.g. with Gaia) comparison to RASS (and other X-ray surveys) long-term variability (baseline 25 years) Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
14 erosita early science - pointings η Cha (B8V) and field (DSS) The η Cha cluster nearby (100 pc) star forming region, intermediate age (5 8 Myr) deep south (-73.5 deg ecl. lat), German half-sky early science and test of field scan mode Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
15 The η Cha cluster The open cluster η Cha: part of Oph-Sco-Cen association (OSCA) SFR with young stars at var. evolutionary stages (CTTS, TO, WTTS) X-ray discovered (ROSAT/HRI), key target (Herschel, HST, Spitzer, XMM...) test case for PMS-evolution, disk dispersal and planet formation dispersed population expected, optical surveys ongoing Why erosita? X-rays are a prime indicator of young stars! (Mamajek et al., 1999) 5 ks depth: log L X lim 27.8 erg s 1 ( 4 x 4 deg, 1 day) 8 ks depth: log L X lim 27.6 erg s 1 ( 4.5 x 4.5 deg, 2 days) free of dark clouds, low absorption detect & characterize stellar population down to low mass regime Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
16 erostars : science projects Hamburg projects/collaborations stellar census - the global view population studies: solar neighborhood, moving groups & SFRs specific objects: ApBp stars, UCDs, planet-bearing stars... the corona-chromosphere connection diffuse stellar components German erosita institutes Tuebingen: young clusters/star-forming regions, BDs (Kavenagh, Whelan) AIP: optical/massive stars (Schnurr) MPE: nucleosynthesis/x-ray bubbles (Diehl) Russian side: stellar working group scheme vague; collaborations very welcome Inter-National: several high-expertise groups expressed interest in erosita Jan Robrade (Hamburger Sternwarte) erosita - StarsWG / 13
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