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Galactic Winds in Dwarf Galaxies?

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Galactic Winds in Dwarf Galaxies? 28.05.2017 Starburst Dwarf Galaxies SS 2017 1 Starburst Dwarf Galaxies The star-formation history does in general not show a continuous evolution but preferably an episoidal behaviour. SS 2017 2 1 28.05.2017 Definition: Starburst (t ) 0 10. ....100 from stellar population synthesis ( G ) M HI HI mass SFR (t ) G Hubble 0 Examples: at former times: Globular Clusters Dwarf Ellipticals giant Ellipticals at present: giant HII regions > 30 Dor SBDGs NGC 1569, NGC 4449, NGC 5253 He 2-10, NGC 1705, III Zw 102 M82, NGC 253 nuclear SBs NGC 1808, NGC 2903, Mkr 297 ULIRGs SSMerger 2017 4 Dwarf Galaxies and Galactic Winds In NGC 1569 2 Super Star Clusters at the base of the gas stream are the engines of the galactic wind due SS 2017 to their5 cumulative supernova II explosions. 2 28.05.2017 Model: • bipolar outflow; • the S part towards observer is unobscured; • disk inclination known. X-ray in colors according to hardness (blue: hard, red: soft) SS 2017 6 overlaid with HI contours (white) Martin et al. (2002) Abundances in the galactic wind from X-ray spectra SS 2017 Martin7 et al. (2002) ApJ 574 3 28.05.2017 The mass loss can be determined from the effective yield yeff of the HI ISM. The loss of metals should be visible in the hot gas outflow. SS 2017 8Martin et al. (2002) ApJ 574 Galactic winds MacLow & Ferrara (1999) courtesy Simone Recchi • Effective yields of dIrrs < solar! • Outflow of SNII gas reduces e.g. O, y SSeff 2017 9 • but: simple outflow models cannot account for gas mixing + turb. heating 4 28.05.2017 Galactic winds in Dwarf Galaxies? Continuous mechanical L over 50 Myrs for various galaxy masses Mg and gas densities n: at t=50 Myrs No consistent star formation! SS 2017 11 MacLow & Ferrara (1999) t=100 Myrs SS 2017 MacLow12 & Ferrara (1999) 5 28.05.2017 Galactic winds in DGs and the fate of metals Luminosity (1038 erg s-1)‏ 0,1 1 10 106 0,18 1 1 1 0,99 1 7 ‏ 10 3.5e-3 8.4e-3 4.8e-2 ) M 1 1 1 108 1.1e-4 3.4e-4 1.3e-3 Mass ( 0,8 1 1 Mass ejection efficiencies Metal ejection efficiencies SS 2017 14 MacLow & Ferrara (1999) Recchi & Hensler (2013) A&A, 551 Testing galactic winds in different gas disks Initial conditions: 7 8 9 • Baryonic mass: Mb = 10 , 10 , 10 M • Stellar disk by Myamoto-Nagai potential • Isothermal gas disk with flattening b/a = 0.2, 1.0, 5.0 • Gas fraction: 60% (L), 90% (H) • Spherical DM halo with MDM = 10 Mb • SFR~2 SS 2017 15 6 28.05.2017 Testing galactic winds in different gas disks (2013) A&A, 551 SN ~ 5% Blow-away of total gas almost impossible: Only in lowest-mass DGs and flat, light gas disks, but then all metals are lost. Gas disk, mixing, turbulence, external halo gas, and embedded clouds hamperSS outflow2017 . 16 Testing galactic winds in different gas disks Oxygen ejection: Only lowest-mass DGs with lower gas fraction lose large O fractions. Thick gas disk and massive DGs retain their supernova elements. Recchi & Hensler (2013) A&A, 551 SS 2017 17 7 28.05.2017 Testing galactic winds in different gas disks ‘H’ models ISM abundances: • The thicker the gas disk, the higher the metal enrichment. • The larger the mass, the larger the metallicity. • The larger the gas content, the greater the metal enrichment. Blow-away of total gas almost impossible: • Only in lowest-mass DGs + flat, light gas disks, lose all metals. • Gas disk, mixing, turbulence, external halo gas, and embedded clouds hamper outflow. SS 2017 18 Can strong Galactic Winds solve the CDM cusp/core problem? Loss of low-ang.mom. gas! (2010) Nature, 463 (2012) MNRAS, 422 NO solution when metal. mismatchSS 2017 ! 20 8 28.05.2017 Large-scale outflows + gas-phase mixing (2006) A&A, 445 In reality: blowaway almost impossible: gas halo, infalling clouds, Timescales of gas return turbulence cooling of blow-out hot gas and fall back: ~ Gyrs turbulent mixing: ~ 20 Myrs metals retained evaporativeSS 2017 mixing: 10 … 100 Myrs (Rieschick21 & G.H. 2002) Refill of Superbubbles Due to cooling and buoyancy the surrounding gas pressure refills the superbubble cave after a few 100 Myrs Recchi et al. (2006) A&A, 445 SS 2017 22 9 28.05.2017 What triggers the high star-formation rates? Gas Infall? Consider the effects of external gas infall! SS 2017 23 Gas Infall to DGs What triggers the high star-formation rates? Consider the effects of SS 2017 external24 gas infall! 10 28.05.2017 Gas infall triggers Starburst The case od NGC 1569: 6 • HI clouds (each ~10 M) fall towards in from a disk • 2 huge super star clusters are formed. (2005, AJ, 130) SS 2017 25 NGC 1569 Gas Infall confirmed! see Muehle et al. (2005) and in many other SBDGs! H HI Stil & Isreal (2002) SS 2017 26 11 28.05.2017 NGC 4449 a triggered starburst SS 2017 27 (Hunter et al. 1995) II Zw 40 SS 2017 (van Zee et al.28 1997 ) 12 28.05.2017 (Östlin & Kunth 2000) I Zw 18 - a perturbed dIrr with gas infall? SS 2017 29 (van Zee et al. 1997) I Zw 18 is associated with a 8.8.7. Associated HI Clouds kinematically disjunct HI complex. SS 2017 30 van Zee et al. (1998) 13 28.05.2017 BCD NGC 1705 SS 2017 31 Dwarf Starburst Galaxies NGC 1705 But: super star cluster are experiencing an epoch not formed in the center of strong Star Formation: • Massive stars illuminate their surrounding gas; • Exploding stars release hot, vehemently expanding gas X-ray contours H overlaid on HI H (Hensler et al. 1997) 2 kpc SS 2017 32 14 28.05.2017 Galactic outflows and infalling clouds Recchi & Hensler (2007) A&A, 477 Although clouds hamper the outflow by evaporated mass-loading, by this, reducing the metal loss, over-running clouds pierce holes into the superbubble shell: nozzle-like outflows are facilitated. SS 2017 33 He 2-10 A dIrr colliding with an intergalactic cloud? Papaderos et al. (1998) Kobulnicky et al. (1995) CO Vacca & Conti (1992) UV V X Hensler et al. (1997) SS 2017 34 15 28.05.2017 Metal differences Metal content of the cool (∼104 K) circumgalactic medium around between 28 HI-selected LLS at z 1 observed in outflow vs. infall absorption against background QSOs SS 2017 35 Star formation is self-regulated! SF = g_cons = Mg/ Hubble or -1 sSFR:= s = /Mgal 0.01 Gyr What triggers high star-formation rates? Gas Infall? The effects of external gas infall vs. outflow! Both act simultaneously: e.g. at high z~2-3: Erb (2008) ApJ, 674 at low z 1: Lehner et al. (2013) ApJ, 770 present: starburst DGs SS 2017 36 16 28.05.2017 Can Gas Infall explain a chemical rejuvenation of dIrrs and their abundance peculiarities ? SS 2017 37 N/O production: • O is produced in massive stars The N/O problem and released by SNeII (hot gas); of dIrrs/BCDs • N is mainly produced in intermediate-mass stars (warm gas); • Massive stars live shorter than Henry, Edmunds, Köppen, (1999) IMS; • N also produced and released by massive stars as primary and secondary element N/O signatures: • HII regions in gSs along second.-N production track; • outer HII regions resemble dIrrs scatter; • dIrrs show low N/O (~ -1.5) at low O! Henry, R.B.C. & Worthey, G. (1999) Stellar evolution tracks pass dIrr regime too fast! SS 2017 38 17 28.05.2017 Gas Infall: its Effect on Abundances Model assumptions: Yields same as in Henry et al. (2000): van der Hoek & Groenewegen (1997), Maeder (1992) Galaxy models evolve for 13 Gyrs with different yeff of 0.1 ... 1 reaching different loc.s in (N/O)-(O/H) diagram Infall of clouds with primordial abund. and 6 8 masses of 10 ... 10 M produces loops. Koeppen & G.H. (2005) A&A, 434 SS 2017 39 Gas Infall and its Effect on Abundances Koeppen & Hensler (2005) A&A, 434 Extension of tracks depends on yeff (N/O) scatter repro- ducible by age diff‘s of start models . SS 2017 40 18 .
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