Ultraluminous X-ray Sources in Nearby Galaxies

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1 Ultraluminous X-ray Sources in Nearby Galaxies Doug Swartz NASA/Marshall Space Flight Center

2 Ultraluminous X-ray Sources in the Universe Doug Swartz NASA/Marshall Space Flight Center

3 Pre-Einstein X-ray Discoveries Uhuru Ariel V

4 Pre-Einstein X-ray Discoveries LMC SMC M Balloon 1971 Uhuru 0.4 x X-1, X-2, X-3, X-4 X Rocket 2.0 x by 1979 by 1984 several transients optical counterparts transients (A ) optical counterparts Helfand PASP 96, 913 (1984)

5 Einstein X-ray Observatory Nov Apr 1981 First imaging X-ray telescope IPC: 60, kev, 100 cm 2 HRI: 5, kev, 25 cm 2 First Guest Observer program mirror assembly

6 Einstein X-ray Observatory Nov Apr 1981 First imaging X-ray telescope IPC: 60, kev, 100 cm 2 HRI: 5, kev, 25 cm 2 First Guest Observer program Local Group: Helfand (1984) 2Ms, ~200 srcs, mostly LMC, M31 (some SMC) Pop.I (HMXB) dominate in late-type galaxies Normal Galaxy Survey: Long & Van Speybroeck (1983) 51/70 detected; Lx ~ Lopt Higher Lx/Lopt in late-type/interacting many `Super-Eddington including six > NGC 2403, M101 (3), NGC 6946, M100 mirror assembly

7 Einstein X-ray Observatory Nov Apr 1981 First imaging X-ray telescope IPC: 60, kev, 100 cm 2 HRI: 5, kev, 25 cm 2 First Guest Observer program Local Group: Helfand (1984) 2Ms, ~200 srcs, mostly LMC, M31 (some SMC) Pop.I dominate in late-type galaxies Normal Galaxy Survey: Long & Van Speybroeck (1983) 51/70 detected; Lx ~ Lopt Higher Lx/Lopt in late-type/interacting many `Super-Eddington including six > NGC 2403, M101 (3), NGC 6946, M100 mirror assembly

8 Einstein X-ray Observatory Luminous X-ray sources are not common objects, perhaps one in 10 9 stellar systems it is useful to study these objects to improve statistical estimates, to better define the extremes of the phenomenon, to determine the dependence upon the stellar population and galactic morphology, and possibly to discover new classes of these rare objects. Long & Van Speybroeck (1983) in Accretion Driven X-ray Sources

9 Einstein X-ray Observatory

10 Einstein X-ray Observatory M81 X-9 (Ho IX X-1) M81 X-6 Fabbiano (1988)

11 ROSAT X-ray Observatory

12 ROSAT X-ray Observatory Colbert & Mushotzky (1999) ROSAT HRI 39 nearby galaxies (6 w/ ASCA spectra) First statement advocating new population: IMBH Roberts & Warwick (2000) ROSAT HRI against 486 dwarf Seyfert catalog (Ho+ 1995) 187 sources in 83 galaxies 27 ULX candidates Colbert & Ptak (2002) ROSAT HRI against RC3 catalog (de Vaucouleurs+ 1991) 87 ULXs in 54 galaxies w/in 2x D25 many are background (Swartz 2006) Liu & Bregman (2005) ROSAT HRI against subset of RC3 106 ULXs w/in D25 in 63 galaxies

13 87 ULX candidates (41 beyond D25) Colbert & Ptak (2002) Swartz (2006)

14 87 ULX candidates (41 beyond D25) Colbert & Ptak (2002) all 25 with spectroscopic redshifts are background Lopez-Corredoira & Gutierrez (2006); Gutierrez & Lopez- Corredoira (2007) Remainder are Fx/Fo~1 (AGN-like) Swartz (2006)

15 Chandra & XMM-Newton Era Vast improvement in angular resolution (Chandra) and effective area (XMM) greatly improves identification of ULX candidates out to 40+ Mpc ; spectra+timing X-ray Luminosity Functions Host Galaxies & Local Environments Specific Frequencies & Scaling Laws

16 X-ray Luminosity Functions The slope, normalization and, if present, breaks & cutoffs in XLFs can constrain accretion scenarios & accretor masses, can distinguish source classes, and can quantify the contribution of ULXs to the luminosity density Spirals: L -0.6 w/ cutoff at 2x10 40, ULX dominate Lx Lx(HMXB)/SFR ~ 2x10 39 /(M /yr) Ellipticals: L -1.5, Lx(LMXB)/M ~ 2x10 39 /(10 10 M ) (Grimm+2003, Swartz+2004,11, Walton+2011, Mineo+2012)

17 Theory of XLF Shapes NS BH IMBH Grimm+ (2003)

18 Observed Luminosity Funtion confidence contours at 1σ, 2σ, 3σ Confidence Contours (counts based luminosities) N(>L) Luminosity/10 39 (erg/s) Exponential Cutoff Luminosity/10 39 (erg/s) Power Law Slope The 3σ range of cut-off luminosity corresponds to solar masses LEdd The normalization of the XLF implies ULXs account for about 5% of CXB ULXs much more luminous than the cut-off must represent a new class of object Swartz+ (2011)

19 Observed Luminosity Funtion confidence contours at 1σ, 2σ, 3σ Confidence Contours (counts based luminosities) N(>L) Luminosity/10 39 (erg/s) Exponential Cutoff Luminosity/10 39 (erg/s) Power Law Slope The 3σ range of cut-off luminosity corresponds to solar masses L Edd The normalization of the XLF implies ULXs account for about 5% of CXB ULXs much more luminous than the cut-off must represent a new class of object Swartz+ (2011)

20 Host Galaxies & Local Environments Host galaxy properties and ULX local environments reveal correlations with underlying stellar population ages, masses, metallicities and star-formation histories Lx~LFIR(~SFR) David Jones & Forman (1992) Einstein+IRAS Individual ULXs e.g., Soria+(2005) Near but not in SSC Zezas&Fabbiano (2002); Kaaret+(2004) SSC ages <6Myr; M Poutanen+(2013) HST+VLT Often in young SF regions Swartz+(2009) Sometimes (11/62) RSG counterparts Heida+(2014) NIR

21 Host Galaxies & Local Environments NGC 4559 X7 ~2x10 40 erg/s F814W HMXB: Myr; M donor; 0.05<Z/Z <0.4 ~ M accretor Soria+(2005) F555W - F814W

22 Host Galaxies & Local Environments SDSS DR6 + local sample ULXs (58 galaxies) NGC 4725 NGC 5585 UGC 8041 NGC 4559 X7 Swartz+(2009)

23 Host Galaxies & Local Environments SDSS DR6 + local sample ULXs (58 galaxies) u -g g -r r -i Can do SED fitting for much larger samples see also Mineo+(2013,2014) on NGC2207 Swartz+(2009)

24 Specific Frequencies & Scaling Laws Ideally, relationships between ULXs and their hosts learned from nearby galaxies extends to more distant and rare environments. Lx /10 39 = 6.7*SFR; universal HMXB XLF Grimm+(2003) Lx /10 39 = 1.8*SFR; + LMXBs Lehmer+(2010) Lx /10 39 = 2.6*SFR; including U/LIRGs Mineo+(2012) Lx /10 39 = 4.0*SFR; to z~1.3 Mineo+(2014) Additional dependencies on choice of SFR proxies, sample differences, absorption, AGN+hot gas

25 Specific Frequencies & Scaling Laws Lx /10 39 = 2.6*SFR extends to LIRGs/ULIRGs and CDF Mineo+(2012)

26 Specific Frequencies & Scaling Laws Lehmer+(2016)

27 Specific Frequencies & Scaling Laws Underluminous due to high column density? see also Luangtip+2014: NULX/SFR=0.2 cf. Swartz+2011 NULX/SFR=2 Lehmer+(2010), Symeonidis+(2011,2014), Iwasawa+(2011), Basu-Zych+(2013), Mineo+(2014)

28 Future Population Studies Big Data & Data Mining Galaxy Evolution Cosmology

29 Recent Big Data Population Studies Utilizing large source catalogs & surveys - good for identifying ULX & extreme HLX candidates 2XMM 320 deg 2, 190k objects (Watson+2009) 3XMM ~700 deg 2, 400k objects (Rosen+2016) CSC v deg 2, 95k objects (Evans+2010) CSC v deg 2, 280k objects (coming in 2016) 2XMM x SDSS/DR7 (Pineau+2011) not ULX-specific 2XMM x RC3 (Walton+2011) 470 ULX candidates 3XMM x SDSS (Zolotukhin+2016) HLX candidates CSC x HyperLEDA (Gong+2016) HLX candidates Chandra x RC3 (S. Wang+2016) not ULX-specific sources in 1110 galaxies!

30 Future Big Data Studies Deep, large-area and full-sky surveys - good for identifying local environments/counterparts SDSS DR deg 2, 470M objects, >22mag ugriz PanSTARRS decl.> o, >24mag grizy (~29mag stacked) LSST 1st light c.2021 El Penon, Chili WISE all-sky (AllWISE: 747M objects) 3.4,4.6,12,22µm FIRST deg 2, 20cm, 1mJy detection threshold erosita 2017 launch, resolution, erg/cm 2 /s, Lx=10 39 out to 30 Mpc, out to 90 Mpc: ~100 ULXs (Prokopenko & Gilfanov 2009)

31 Galaxy Evolution Expect ULXs to play a role in feedback because their radiative and mechanical power rivals that of other stellar sources XLF slope implies a few ULXs dominate total Lx ULXs turn on >10Myr after start of SF; Δt~1Myr SNe kicks place active XRBs outside clusters, in cold ISM

32 Galaxy Evolution Observed properties (Feng&Soria2011 review) ULX bubbles up to 100 s pc Pakull&Mirioni (2002,2003) Lmech ~ erg/s; L*Δt ~ erg (100 SNe) jets Lmech >> Lx Pakull+(2011) HoIX X-1 Pakull&Grise(2008) NGC7793 S26 Soria+(2010)

33 Cosmology Predictions from population synthesis + cosmological simulations New players in the scaling relation: redshift z (stellar age, SF history), Z/Z Feedback enhanced in early universe: more & brighter HMXBs aid reionization Brorby+(2014,2015), Justham&Schawinski(2015), Linden+(2010)

34 Cosmology HMXBs: peaks where Z/Z is lowest LMXBs: peaks where RG donor mass is ~3 M Fragos+(2013)

35 Cosmology LLMXB/M ~ (1+z) 2 or 3 (younger host galaxy stellar age) LHMXB/SFR ~ (1+z) (lower metallicity) HMXB > AGN at z>5 Lehmer+(2016) arxiv:

36 Future Population Studies X-ray Surveyor x more EA than Chandra, 500x survey speed (4Ms CDF in 80ks) erg/s in 4Ms <1 resolution Vikhlinen+(2015)

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