X-Rays and the Effelsberg Telescope Jrn Wilms Dr. Remeis-Sternwarte - PowerPoint PPT Presentation

X-Rays and the Effelsberg Telescope Jörn Wilms Dr. Remeis-Sternwarte & ECAP in collaboration with: Julia C. Lee (Harvard), M.A. Nowak (MIT), N.S. Schulz (MIT), R. Smith (CfA), Lia Corrales (Michigan), T. Kallman (GSFC), E. Gatuzz (ESO), J. García (Caltech), Annika Kreikenbohm (Würzburg/ECAP), Mirjam Örtel (ECAP), Sara Rezaei Khoshbakht (MPIA)

Life of an X-ray astronomer Typical life of an X-ray astronomer: solaris:~/data > make proposal

Life of an X-ray astronomer Typical life of an X-ray astronomer: solaris:~/data > make proposal linux:~/data > make observation

Life of an X-ray astronomer Typical life of an X-ray astronomer: solaris:~/data > make proposal linux:~/data > make observation macos:~/data > make datareduction

Life of an X-ray astronomer Typical life of an X-ray astronomer: solaris:~/data > make proposal linux:~/data > make observation macos:~/data > make datareduction Lookup 21 cm N H macos:~/data > nh ⇐ =

Life of an X-ray astronomer Typical life of an X-ray astronomer: solaris:~/data > make proposal linux:~/data > make observation macos:~/data > make datareduction Lookup 21 cm N H macos:~/data > nh ⇐ = macos:~/data > xspec Xspec 15.3.55 21:14:59 05-Oct-2029 For documentation, notes, and fixes see http://xspec.gsfc.nasa.gov/ Plot device not set, use "cpd" to set it Type "help" or "?" for further information XSPEC > data athena_xifu.pha

Life of an X-ray astronomer Typical life of an X-ray astronomer: solaris:~/data > make proposal linux:~/data > make observation macos:~/data > make datareduction Lookup 21 cm N H macos:~/data > nh ⇐ = macos:~/data > xspec Xspec 15.3.55 21:14:59 05-Oct-2029 For documentation, notes, and fixes see http://xspec.gsfc.nasa.gov/ Plot device not set, use "cpd" to set it Type "help" or "?" for further information XSPEC > data athena_xifu.pha This is why I’m giving this talk (Wilms et al., 2000) XSPEC > model tbabs*power ⇐ =

ISM and X-rays (Snowden et al., 1997) Diffuse emission in the X-rays: ROSAT All Sky Survey (1990s) (will soon be superseded by eROSITA)

ISM and X-rays (Snowden et al., 1997) Diffuse emission in the X-rays: ROSAT All Sky Survey (1990s) (will soon be superseded by eROSITA)

ISM and X-rays (Snowden et al., 1997) Diffuse emission in the X-rays: ROSAT All Sky Survey (1990s) (will soon be superseded by eROSITA)

ISM and X-rays (Voges et al., 1999) Source spectra of bright sources in the ROSAT All Sky Survey

ISM and X-rays

ISM and X-rays 10 +1 F E [arbitrary units] 10 +0 10 − 1 10 − 2 10 − 3 0.5 1 2 5 10 Energy [keV]

ISM and X-rays 10 +1 F E [arbitrary units] 10 +0 10 − 1 10 − 2 10 − 3 0.5 1 2 5 10 Energy [keV]

ISM and X-rays 10 +1 F E [arbitrary units] 10 +0 10 − 1 10 − 2 10 − 3 0.5 1 2 5 10 Energy [keV]

ISM and X-rays 10 +1 F E [arbitrary units] 10 +0 10 − 1 10 − 2 10 − 3 0.5 1 2 5 10 Energy [keV]

ISM and X-rays 10 +1 F E [arbitrary units] 10 +0 10 − 1 10 − 2 10 − 3 0.5 1 2 5 10 Energy [keV]

ISM and X-rays 10 +1 10 +1 F E [arbitrary units] F E [arbitrary units] 10 +0 10 +0 10 − 1 10 − 1 10 − 2 10 − 2 10 − 3 10 − 3 0.5 1 2 5 10 0.5 1 2 5 10 Energy [keV] Energy [keV]

ISM and X-rays ISM 10 +1 10 +1 F E [arbitrary units] F E [arbitrary units] 10 +0 10 +0 10 − 1 10 − 1 10 − 2 10 − 2 10 − 3 10 − 3 0.5 1 2 5 10 0.5 1 2 5 10 Energy [keV] Energy [keV]

ISM and X-rays 10 +1 F E [arbitrary units] 10 +0 ISM 10 − 1 10 +1 10 +1 F E [arbitrary units] F E [arbitrary units] 10 − 2 10 +0 10 +0 10 − 1 10 − 1 10 − 3 10 − 2 10 − 2 0.5 1 2 5 10 10 − 3 10 − 3 0.5 1 2 5 10 0.5 1 2 5 10 Energy [keV] Energy [keV] Energy [keV] � � � F obs ( E ) = exp − N H A Z σ bf,Z ( E ) F source ( E ) Z

ISM and X-rays Wavelength [˚ A] Photoabsorption strongly modifies the 100 10 1 observed X-ray spectrum 100 F obs ( E ) = e ( − N H Z A Z σ bf,Z ( E ) ) F src ( E ) � Observed flux [ph cm − 2 s − 1 keV − 1 ] 3 10 19 • “Hydrogen column”: 1 10 20 10 � ℓ 3 10 20 n p ( r ) d r N H = 0 1 10 21 where n p proton (!) particle density, 1 3 10 21 often taken from LAB-survey and successors. 1 10 22 • σ bf,Z : photoabsorption cross section 0.1 3 10 22 ⇒ ionization state! = • A Z : elemental abundance by num- ber (wrt Hydrogen) 0.01 0.1 1 10 Energy [keV]

Cross sections 0.1 1.0 10.0 Ni 700 Fe 10 −1 10 −2 σ [Mbarn/H] 600 10 −3 10 −4 400 keV [10 −24 cm 2 ] 10 −5 Cr 10 −6 Ar Ca 300 0.1 1.0 10.0 S E [keV] Si σ E 3 MgAl 200 Ne Fe−L N O 100 C H+He H 2 H 0.1 1.0 10.0 E [keV] N H is used to describe the column, but X-rays measure the metal col- umn. ⇒ Need very good knowledge of cross sections = ⇒ Knowing abundances is important to be able to compare X-ray N H = w/ N H from other wavebands (21 cm!!) Radio- N (21 cm): only neutral !

O Energy [keV] 0.60 0.58 0.56 0.54 0.52 0.50 0.48 O K edge Photon flux [arbitrary units] 10 − 1 10 − 2 10 − 3 10 − 4 10 − 5 10 − 6 21.0 22.0 23.0 24.0 25.0 26.0 Wavelength [˚ A] Oxygen: Gorczycka; note resonance absorption line

O 5 O I 1s−2p Flux (10 −5 f.u.) 2 1 O II 0.5 O III Counts (per bin) 20 10 0 1 χ −1 0 22 24 26 Wavelength [Å] Oxygen: Gorczycka; note resonance absorption line Data: Cyg X-1 (Hanke et al., 2009)

Fe Energy [keV] 0.78 0.76 0.74 0.72 0.70 3.0 Fe L edge Photon flux [arbitrary units] 2.5 2.0 1.5 1.0 0.5 15.5 16.0 16.5 17.0 17.5 18.0 Wavelength [˚ A] Iron: Brennan & Cowan (1992), Kortright & Kim (2000) (note: solid state ef- fects)

Fe Flux (10 −5 f.u.) 2 Fe L 3 Fe L 2 1 Counts (per bin) 20 10 2 χ 0 −2 17 17.5 18 Wavelength [Å] Iron: Brennan & Cowan (1992), Kortright & Kim (2000) (note: solid state ef- fects) Data: Cyg X-1 (Hanke et al., 2009)

Abundances 12 Anders & Grevesse (1989) Lodders (2003) Asplund et al. (2009) 10 Wilms et al. (1999) log Abundance (H=12) 8 6 4 2 H Li B N F Na Al P Cl K Sc V Mn Co Cu He Be C O Ne Mg Si S Ar Ca Ti Cr Fe Ni Best current values for Sun : Asplund et al. (2009). but ISM is different = ⇒ potential for systematic error

Abundances 2.0 Anders & Grevesse (1989) Lodders (2003) Asplund et al. (2009) 1.8 Abundance/(Wilms et al., 1999) 1.6 1.4 1.2 1.0 0.8 H He Li Be B C N O F NeNaMgAl Si P S Cl Ar K CaSc Ti V CrMnFeCoNiCu “Solar abundances” of Anders & Grevesse (1989): ∼ 40% higher than ISM and ∼ 20% higher than modern solar abundance.

Abundances 2.0 Anders & Grevesse (1989) Lodders (2003) Asplund et al. (2009) 1.8 Abundance/(Wilms et al., 1999) 1.6 1.4 1.2 1.0 0.8 H He Li Be B C N O F NeNaMgAl Si P S Cl Ar K CaSc Ti V CrMnFeCoNiCu Rule of thumb: N H from LAB-survey, Wilms et al. (2000) ISM abun- dances, describes X-ray absorption well ( ± 10%). ⇒ This is why LAB-survey is crucial for X-ray astronomy. =

σ σ Ionization 0.06 ISMABS TBNew 0.05 Photons cm -2 s -1 Å -1 0.04 0.03 0.02 0.01 O K region 0.00 25 0 σ -25 21 21.5 22 22.5 23 23.5 24 0.10 Wavelength (Å) ISMABS 0.09 TBNew Photons cm -2 s -1 Å -1 0.08 High resolution spectra show influ- 0.07 0.06 ence of ionized ISM 0.05 0.04 Ne K region 0.03 0.02 25 0 ⇒ ISMabs model (Gatuzz et al., σ = -25 2015) 13 13.5 14 14.5 15 0.070 σ σ

Dust extinction (Hanke, 2011) Dust scattering out of line of sight: Extinction versus absorption (e.g., Corrales et al., 2016; Smith et al., 2016; Hoffman & Draine, 2016)

Dust extinction (Corrales et al., 2016) Dust scattering out of line of sight: Extinction versus absorption (e.g., Corrales et al., 2016; Smith et al., 2016; Hoffman & Draine, 2016)

Structure of the ISM Gatuzz et al. (submitted) – XMM-Newton pointings, Gaia distances

Structure of the ISM Gatuzz et al. (submitted)

Structure of the ISM Optical extinction map (Capitanio et al., 2017) X-rays (Gatuzz et al.)

eROSITA ⇒ Spectr-RG : = • X-ray all sky survey (4 years) • most sensitive AGN sur- vey (2 × 10 6 ) • 100000 clusters • Instruments: – eROSITA : Germany (MPE et al.) – ART-XC : Roscosmos • Launch: 2018/2019, Duration > 7 years Spectrum-X- Γ

Athena • Next large X-ray mission of ESA (ESA, 10 8 Euro) • Launch 2030 • Instruments: – WFI : Wide field Instrument – X-IFU : High resolution calorimeter

Summary • Knowledge of N H crucial for X-ray data analysis ⇒ importance of 21 cm surveys = • high SNR X-ray observations provide complementary information to 21 cm: metal distribution, ionization. The future here is very bright with XARM (2022), Athena (2030), and perhaps Arcus (2025) • Can now start to reconstruct 3D structure of ISM by combining 21 cm, Gaia, X-ray ⇒ eROSITA =