AN UNIDENTIFIED X-RAY LINE IN ANDROMEDA, PERSEUS AND THE GALACTIC CENTER
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1 AN UNIDENTIFIED X-RAY LINE IN ANDROMEDA, PERSEUS AND THE GALACTIC CENTER Jeroen Franse Instituut Lorentz & Leiden Observatory COSMO August 26, Chicago JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 1 / 16
2 INTRODUCTION & MOTIVATION DETECTION OF AN UNIDENTIFIED LINE JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 2 / 16
3 INTRODUCTION & MOTIVATION DARK MATTER CANDIDATE: WIMP Weakly Interacting Massive Particle Interaction strength as Weak force Produced at correct Ω DM for GeV - TeV masses JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 3 / 16
4 INTRODUCTION & MOTIVATION DARK MATTER CANDIDATE: WIMP Weakly Interacting Massive Particle Interaction strength as Weak force Short lifetime Produced at correct Ω DM for GeV - TeV masses Cold DM JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 3 / 16
5 INTRODUCTION & MOTIVATION DARK MATTER CANDIDATE: WIMP Weakly Interacting Massive Particle Interaction strength as Weak force Short lifetime Produced at correct Ω DM for GeV - TeV masses To be DM, must be made stable with new physics Cold DM JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 3 / 16
6 INTRODUCTION & MOTIVATION DARK MATTER CANDIDATE: SUPERWIMP Super-Weakly Interacting Massive Particle Lower interaction strength Lower mass for correct Ω DM JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 4 / 16
7 INTRODUCTION & MOTIVATION DARK MATTER CANDIDATE: SUPERWIMP Super-Weakly Interacting Massive Particle Lower interaction strength Longer lifetime Lower mass for correct Ω DM Warmer DM JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 4 / 16
8 INTRODUCTION & MOTIVATION DARK MATTER CANDIDATE: SUPERWIMP Super-Weakly Interacting Massive Particle Lower interaction strength Longer lifetime Lower mass for correct Ω DM Can be DM if lifetime > lifetime of the universe Warmer DM Is allowed to decay JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 4 / 16
9 INTRODUCTION & MOTIVATION DARK MATTER SUPERWIMPS IN X-RAYS Decaying dark matter should decay into X-rays JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 5 / 16
10 I NTRODUCTION & M OTIVATION X- RAYS P OTENTIAL TARGET S OURCES Dark matter dominated objects. Specifically, sources with high expected decay signal strength signal DM mass in FoV / distance2 J EROEN F RANSE I NSTITUUT L ORENTZ & L EIDEN O BSERVATORY COSMO AUGUST 26, C HICAGO 6 / 16
11 I NTRODUCTION & M OTIVATION X- RAYS P OTENTIAL TARGET S OURCES Dark matter dominated objects. Specifically, sources with high expected decay signal strength signal DM mass in FoV / distance2 Typical cluster spectrum Werner et al J EROEN F RANSE I NSTITUUT L ORENTZ & L EIDEN O BSERVATORY COSMO AUGUST 26, C HICAGO 6 / 16
12 DATA DATA OUR DATA M31 GALAXY XMM-Newton, center & outskirts PERSEUS CLUSTER XMM-Newton, outskirts only GALACTIC CENTER XMM-Newton, inner 50pc BLANK SKY XMM-Newton BULBUL ET AL CLUSTERS XMM-Newton, centers only Up to z = 0.35, including Coma, Perseus PERSEUS CLUSTER Chandra, center only VIRGO CLUSTER Chandra, center only JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 7 / 16
13 DETECTION DETECTION AT E 3.5 KEV Andromeda (M31) JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 8 / 16
14 DETECTION DETECTION AT E 3.5 KEV Galactic Center JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 9 / 16
15 DETECTION SIGNIFICANCES OUR DATA PERSEUS + M31 4.4σ GALACTIC CENTER 5.7σ BLANK SKY No detection BULBUL ET AL FULL MOS 5σ FULL PN 4σ PERSEUS ACIS-S 3.4σ PERSEUS ACIS-I 2.5σ VIRGO ACIS-I No detection JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 10 / 16
16 LINE ORIGIN INSTRUMENTAL ORIGIN? Instrumental origin unlikely Detected in 4 different detectors Line redshifts correctly with sources Not detected in blank sky dataset More tests in future work More single objects at different redshifts Pure powerlaw objects (Supernova remnants, AGN) JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 11 / 16
17 LINE ORIGIN ATOMIC LINE? Unlikely: can not explain consistently all observations Bulbul et al M31 line is stronger than other atomic emission GC K XVIII origin can not be excluded CLUSTERS need anomalous line ratios of a factor (but see Jeltema & Profumo 2014, arxiv: ) JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 12 / 16
18 LINE ORIGIN DARK MATTER DECAY? The line flux should be directly proportional to DM mass JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 13 / 16
19 LINE ORIGIN DARK MATTER DECAY? The line flux should be directly proportional to DM mass JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 13 / 16
20 LINE ORIGIN COUNTERCLAIMS D. Malyshev, A. Neronov, and D. Eckert: Constraints on 3.55 kev line emission from stacked observations of dwarf spheroidal galaxies [arxiv: ] DM origin marginally excluded M.E. Anderson, E. Churazov, J.N. Bregman: Non-Detection of X-Ray Emission From Sterile Neutrinos in Stacked Galaxy Spectra [arxiv: ] DM origin excluded by up to 11σ JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 14 / 16
21 LINE ORIGIN COUNTERCLAIMS D. Malyshev, A. Neronov, and D. Eckert: Constraints on 3.55 kev line emission from stacked observations of dwarf spheroidal galaxies [arxiv: ] DM origin marginally excluded M.E. Anderson, E. Churazov, J.N. Bregman: Non-Detection of X-Ray Emission From Sterile Neutrinos in Stacked Galaxy Spectra [arxiv: ] DM origin excluded by up to 11σ Errors are underestimated? JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 14 / 16
22 NEXT STEPS WHAT IS NEXT? CURRENT WORK Robust dark matter masses More archival data Cross-correlation of X-ray with dark matter maps Expected decay signals from cosmological simulations FUTURE WORK Spectrally resolve the line with Astro-H (2015) measure velocity dispersion distinguish from K and Ar lines Proposals for new observations JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 15 / 16
23 SUMMARY SUMMARY the signal is still consistent with dark matter there is no satisfying normal explanation consistent with all measurements JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 16 / 16
24 JELTEMA & PROFUMO M31 Fitting the powerlaw only to 3 4 kev JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 16 / 16
25 PROFILES JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 16 / 16
26 PROFILES JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 16 / 16
27 PARAMETER SPACE JEROEN FRANSE INSTITUUT LORENTZ & LEIDEN OBSERVATORY COSMO AUGUST 26, CHICAGO 16 / 16
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