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Explore role of feedback in enriching elements in cosmic phenomena such as supernova remnants, clusters of galaxies, and AGN outflows, providing insights into element distribution and galactic evolution. Learn about nucleosynthesis, galaxy interactions, and the circulation of elements through various processes. This study unlocks the secrets of cosmic element enrichment.
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Feedback and enrichment from SNR to LSS Jelle S. Kaastra SRON
Earth versus solar system Earth Solar system
Which elements can we see? K-shell
Which elements will we see?(IXO) K-shell
Intermediate mass stars • Stars < 8 Msun in late stages produce much C and N through nuclear fusion • strong winds blow elements away • Finally, core collapses to white dwarf and planetary nebula is ejected
Type Ia supernova remnants • Metals are ejected into the interstellar medium • Mainly heavier elements (Si, Fe, Ni) • Example: Cassiopeia B (better known as Tycho, remnant of SN that exploded 1572)
Core collapse remnants • Metals are ejected into the interstellar medium • Mainly lighter elements (O, Ne, Si) • During explosion also nucleosynthesis of heavier metals (up to U) • Example: Cassiopeia A (remnant of SN that exploded ca. 1680) All X-rays Si Ca Fe
Importance clusters of galaxies for abundance studies • Largest bound structures • Fair samples of the Universe • Deep potential wells, retains most of the gas • Hot gas: no significant “hiding” of metals in dust (& more gas than stars) • Spatial extent allows mapping
Simulations • Sample: extended HIFLUCS sample 106 clusters (Reiprich & Böhringer) • Use T & n profiles • Fit multi-T model • Spectra r<0.2R500
Simulations: 10 best cases • Sample: 10th best in 100 ks • WFI: errorsdominatedbysystematics, equalto XMM/EPIC! • NEED High-res! • XMS: unambiguousdetectionall C-Zn (inc. Scandium) • Maps: 0.01 solar in coreforall elements nowdetectedwith XMM
How to get metals in custers?Ram pressure stripping • Ram pressure stripping mostly in cluster cores
Galactic winds • Massive stars born in groups • Sometimes many SN explosions in relatively short time • Combined power may blow gas out of galaxies M 82, optical M 82, X-ray
Galaxy-Galaxy interactions • Close encounters may cause tidal tails • Stars and gas torn away from galaxies • Enriched gas enters intergalactic space Antennae (Sky & Telescope)
Giant outflows from active galaxies • In compact clusters like M87, radio lobes show cool, enriched material levitated by the AGN outflow X-ray Radio
Uplift of enrichedmaterial in M87/Virgo(Simionescu et al. 2008) • Currently only maps in Fe • Need mapping in more elements to reconstruct the source of the metals
Need for mapping different elements • White contours: ram-pressure stripping • Black contours: galactic winds • (after Schindler & Diaferio 2008)
Importance of AGN outflows(adapted from talk Jerry Kriss @ Utrecht conference) • May affect dispersal heavy elements into IGM & ICM (e.g. Cavaliere et al. 2002; Scannapieco & Oh 2004) • Influence ionisation structure IGM (Kriss et al. 1997) • Intertwined with evolution host galaxy (e.g. Silk & Rees 1998; Wyithe & Loeb 2003) • Not sure about how outflows created, their structure, mass & energy: key question: do outflows escape confines of host galaxy? • Crucial to understand working central engine: central engine, energy budget • Low-z AGN are the nearest & brightest, so best objects to study
Complex velocity structure • Example: STIS spectra NGC 5548 (Crenshaw & Kraemer 1999) show 5 velocity components: • Nr 1 high -1040 km/s • Nr 2 med -667 km/s • Nr 3 med -530 km/s • Nr 4 med -336 km/s • Nr 5 low -160 km/s Radial velocity (km/s)
Complex ionisation structure • Gas at multiple ionisation parameters • Hot debate: continuous distribution, or multiple (2 or 3) discrete components in pressure equilibrium? Steenbrugge et al. 2005
Mrk 509 campaign • 600 ks RGS+EPIC+OM XMM-Newton = 10 x 60 ks, 4 days spacing • Simultaneous Integral, 1.2 Ms • Chandra LETGS 170 ks + HST/COS spectra • Swift monitoring in between & before • Optical/IR coverage WHT & Pairitel • One of biggest campaigns on AGN ever
Discrete versus continuous absorption measure distribution? • Column densities well approximated by sum 5 components • Higher column for higher ionisation parameter • But what about a continuous model?
Continuous model(Detmers et al. 2011) • Fitted columns with continuous (spline) model • Surprise comps C & D pop-up as discrete components! • Upper limits FWHM 35 & 80 % • Component B (& A) too poor statistics to prove if continuous • Component E also poorer determined: correlation ξ and NH. D E C B
Ionisation equilibrium E D C B A
Abundances AGN • AGN outflows have chemical composition core galaxy (modified by AGN environment, star formation?) • Hard to measure in emission (systematics, multi-region, etc.) • Mrk 509 results (Steenbrugge et al. 2011): accurate (down to 5 %) abundances of C, N, O, Ne, Mg, Fe
Prospects IXO • Gratings: area & resolution 10 x RGS • 600 ks RGS is 6 ks IXO for weak lines • time-resolved spectroscopy, excellent velocity separation (100 km/s) • XMS: area 100 x RGS, resolution ~ RGS • 600 ks RGS is 6 ks IXO for weak lines • time-resolved spectroscopy
Conclusions • Feedback & chemical enrichment can be studied on all scales with IXO • High-resolution X-ray spectroscopy is the key to all the answers • Let's make that key!