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 macos:~/data> nh ⇐ = Lookup 21 cm 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 macos:~/data> nh ⇐ = Lookup 21 cm 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 macos:~/data> nh ⇐ = Lookup 21 cm 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 XSPEC>model tbabs*power ⇐ = This is why I’m giving this talk (Wilms et al., 2000)

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(will soon be superseded by eROSITA)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(will soon be superseded by eROSITA)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(will soon be superseded by eROSITA)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

5 2 0.5 10 1 10+1 10+0 10−1 10−2 10−3 Energy [keV] FE [arbitrary units]

ISM and X-rays

5 2 0.5 10 1 10+1 10+0 10−1 10−2 10−3 Energy [keV] FE [arbitrary units]

ISM and X-rays

5 2 0.5 10 1 10+1 10+0 10−1 10−2 10−3 Energy [keV] FE [arbitrary units]

ISM and X-rays

5 2 0.5 10 1 10+1 10+0 10−1 10−2 10−3 Energy [keV] FE [arbitrary units]

ISM and X-rays

5 2 0.5 10 1 10+1 10+0 10−1 10−2 10−3 Energy [keV] FE [arbitrary units]

ISM and X-rays

5 2 0.5 10 1 10+1 10+0 10−1 10−2 10−3 Energy [keV] FE [arbitrary units] 5 2 0.5 10 1 10+1 10+0 10−1 10−2 10−3 Energy [keV] FE [arbitrary units]

ISM and X-rays

ISM

5 2 0.5 10 1 10+1 10+0 10−1 10−2 10−3 Energy [keV] FE [arbitrary units] 5 2 0.5 10 1 10+1 10+0 10−1 10−2 10−3 Energy [keV] FE [arbitrary units]

ISM and X-rays

ISM

5 2 0.5 10 1 10+1 10+0 10−1 10−2 10−3 Energy [keV] FE [arbitrary units]

Fobs(E) = exp

• −NH
• Z

AZσbf,Z(E)

• Fsource(E)

5 2 0.5 10 1 10+1 10+0 10−1 10−2 10−3 Energy [keV] FE [arbitrary units]

5 2 0.5 10 1 10+1 10+0 10−1 10−2 10−3 Energy [keV] FE [arbitrary units]

ISM and X-rays

3 1022 1 1022 3 1021 1 1021 3 1020 1 1020 3 1019

10 1 0.1 100 10 1 0.1 0.01 100 10 1 Energy [keV] Observed flux [ph cm−2 s−1 keV−1] Wavelength [˚ A]

Photoabsorption strongly modifies the

• bserved X-ray spectrum

Fobs(E) = e(−NH

• Z AZσbf,Z(E))Fsrc(E)
• “Hydrogen column”:

NH = ℓ np(r) dr where np proton (!) particle density,

• ften taken from LAB-survey and

successors.

• σbf,Z: photoabsorption cross section

= ⇒ ionization state!

• AZ: elemental abundance by num-

ber (wrt Hydrogen)

Cross sections

0.1 1.0 10.0 E [keV] 100 200 300 400 C N O Ne MgAl Si S Ar Ca Cr Fe−L H H+He H2 0.1 1.0 10.0 700 600 σ E3

keV [10−24 cm2]

Fe Ni 0.1 1.0 10.0 E [keV] 10−6 10−5 10−4 10−3 10−2 10−1 σ [Mbarn/H]

NH 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 NH w/NH from other wavebands (21 cm!!)

Radio-N (21 cm): only neutral!

O

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

Oxygen: Gorczycka; note resonance absorption line

O

1 0.5 2 5 Flux (10−5 f.u.) O I 1s−2p

O II O III

10 20 Counts (per bin) 22 24 26 −1 0 1 χ Wavelength [Å]

Oxygen: Gorczycka; note resonance absorption line Data: Cyg X-1 (Hanke et al., 2009)

Fe

18.0 17.5 17.0 16.5 16.0 15.5 3.0 2.5 2.0 1.5 1.0 0.5 0.78 0.76 0.74 0.72 0.70 Wavelength [˚ A] Photon flux [arbitrary units] Energy [keV] Fe L edge

Iron: Brennan & Cowan (1992), Kortright & Kim (2000) (note: solid state ef- fects)

Fe

1 2 Flux (10−5 f.u.)

Fe L2 Fe L3

10 20 Counts (per bin) 17 17.5 18 −2 2 χ Wavelength [Å]

Iron: Brennan & Cowan (1992), Kortright & Kim (2000) (note: solid state ef- fects) Data: Cyg X-1 (Hanke et al., 2009)

Abundances

2 4 6 8 10 12 log Abundance (H=12) H He Li Be B C N O F Ne Na Mg Al Si P S Cl Ar K Ca Sc Ti V Cr Mn Fe Co Ni Cu Anders & Grevesse (1989) Lodders (2003) Asplund et al. (2009) Wilms et al. (1999)

Best current values for Sun: Asplund et al. (2009).

but ISM is different = ⇒ potential for systematic error

Abundances

0.8 1.0 1.2 1.4 1.6 1.8 2.0 Abundance/(Wilms et al., 1999) H He Li Be B C N O F NeNaMgAl Si P S Cl Ar K CaSc Ti V CrMnFeCoNiCu Anders & Grevesse (1989) Lodders (2003) Asplund et al. (2009)

“Solar abundances” of Anders & Grevesse (1989): ∼40% higher than ISM and ∼20% higher than modern solar abundance.

Abundances

0.8 1.0 1.2 1.4 1.6 1.8 2.0 Abundance/(Wilms et al., 1999) H He Li Be B C N O F NeNaMgAl Si P S Cl Ar K CaSc Ti V CrMnFeCoNiCu Anders & Grevesse (1989) Lodders (2003) Asplund et al. (2009)

Rule of thumb: NH 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.

Ionization

σ σ 0.00 0.01 0.02 0.03 0.04 0.05 0.06 Photons cm-2 s-1 Å-1

O K region

ISMABS TBNew

• 25

25 21 21.5 22 22.5 23 23.5 24 σ Wavelength (Å) 0.02 0.03 0.04 0.05 0.06 0.07 0.08 0.09 0.10 Photons cm-2 s-1 Å-1

Ne K region

ISMABS TBNew

• 25

25 13 13.5 14 14.5 15 σ 0.070 σ σ

High resolution spectra show influ- ence of ionized ISM = ⇒ISMabs model (Gatuzz et al., 2015)

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

Spectrum-X-Γ

= ⇒ Spectr-RG:

• X-ray all sky survey

(4 years)

• most sensitive AGN sur-

vey (2 × 106)

• 100000 clusters
• Instruments:

– eROSITA: Germany (MPE et al.) – ART-XC: Roscosmos

• Launch: 2018/2019,

Duration >7 years

Athena

• Next large X-ray mission of ESA (ESA,

108 Euro)

• Launch 2030
• Instruments:

– WFI: Wide field Instrument – X-IFU: High resolution calorimeter

Summary

• Knowledge of NH 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

Bibliography 38a Anders E., Grevesse N., 1989, Geochim. Cosmochim. Acta 53, 197 Asplund M., Grevesse N., Sauval A.J., Scott P., 2009, Ann. Rev. Astron. Astrophys. 47, 481 Brennan S., Cowan P.L., 1992, Rev. Sci. Instrum. 63, 850 Capitanio L., Lallement R., Vergely J.L., et al., 2017, In: Reylé C., Di Matteo P., Herpin F., Lagadec E., Lançon A., Meliani Z., Royer F. (eds.) SF2A-2017: Proceedings

• f the Annual meeting of the French Society of Astronomy and Astrophysics., p.273

Corrales L.R., García J., Wilms J., Baganoff F., 2016, Mon. Not. R. Astron. Soc. 458, 1345 Gatuzz E., García J., Kallman T.R., et al., 2015, Astrophys. J. 800, 29 Hanke M., 2011, Ph.D. thesis, Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Hanke M., Wilms J., Nowak M.A., et al., 2009, Astrophys. J. 690, 330 Hoffman J., Draine B.T., 2016, Astrophys. J. 817, 139 Kortright J.B., Kim S., 2000, Phys. Rev. B 12216 Smith R.K., Valencic L.A., Corrales L., 2016, Astrophys. J. 818, 143 Snowden S.L., Egger R., Freyberg M.J., et al., 1997, Astrophys. J. 485, 125 Voges W., Aschenbach B., Boller T., et al., 1999, Astron. Astrophys. 349, 389 Wilms J., Allen A., McCray R., 2000, Astrophys. J. 542, 914