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Home , Draco (constellation), Leo II (dwarf galaxy), Leo IV (dwarf galaxy), Leo T (dwarf galaxy), Triangulum II

Dark Matter Searches using Dwarf with HAWC

Tolga Yapıcı

11 August 2017

Tolga Yapıcı Searches with HAWC TeVPA 2017, 11 August 2017 1 / 17 LAVA

HAWC Utility Building Counting House

Located at 97.5○ W, 18.9 ○ N (Parque Nacional Pico de Orizaba) at 4100m 300x 7.3 m diameter, 5 m height tanks, 3x 8” R5912 PMTs and 1x 10” R7081-HQE PMT in total: 55kT of water (110 B747s, 160M water bottles) - 3900 truck trips covers 22000 m2, total length of coaxial cables: ∼180km 24kHz trigger rate, 2TB of data per day, 95% livetime

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 2 / 17 The event rate: 20 kHz [data rate of ∼0.02 GB/s (2 TB/day)] Crab : 400 photons/day, Background: 15000 cosmic rays/second

Lots of background, Efficient Background rejection required

[arXiv:1701.01778]

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 3 / 17 Dark Matter Detection

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 4 / 17 Dark Matter Detection

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 5 / 17 Dark Matter - Indirect Detection

Particle Physics Astrophysics

dφ < σv > dN 2 ∝ dΩ ρ dx 2 S Sl.o.s. dE annihilation Mχ dE dφ 1 dN ∝ S dΩ S ρdx dE decay τMχ dE l.o.s.

- Particle Physics part by PYTHIA8 - Astrophysics Part (J- and D- factors) by CLUMPY and references

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 6 / 17 Draco II II Draco WillmanUrsa Major I I AWM 7

Triangulum II CanesCanes Venatici Venatici I II Coma

Coma Berenices II Segue II M31 Laevens 3 Bootes III Segue I Bootes III M49 II NGC 4636 PRELIMINARYLeo IV

Sagittaruis II GC Sagittarius II -60 ◦ -30 ◦ 0 ◦ 30 ◦ 0 ◦ -30 ◦ Fornax-60 ◦

Centaurus II Pictoris I I Eridanus III II ReticulumHorologium II I II Potential sources to look for dark matter signature

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 7 / 17 J- and D- factors (1)

Source RA Dec log10[J(θ)] log10[D(θ)] θmax (deg) (deg) (GeV2cm−5sr) (GeV2cm−2sr) (deg) Bootes 1 210.05 14.49 18.47 18.45 0.47 CanesVenatici I 202.04 33.57 17.62 17.55 0.53 CanesVenatici II 194.29 34.32 17.95 17.69 0.13 186.74 23.90 19.32 18.71 0.31 Draco 260.05 57.07 19.37 19.15 1.30 Hercules 247.72 12.75 16.93 16.89 0.28 Leo I 152.11 12.29 17.57 18.05 0.45 Leo II 168.34 22.13 18.11 17.36 0.23 Leo IV 173.21 -0.53 16.37 16.48 0.16 151.75 16.06 19.66 18.64 0.35 Sextans 153.28 -1.59 17.96 18.48 1.70 II[∗] 33.33 36.18 20.44 18.42 0.12 Ursa Major I 158.72 51.94 19.67 19.04 0.53 Ursa Major II 132.77 63.11 18.66 17.78 0.43 Ursa Minor 227.24 67.24 19.24 18.13 1.37

From different realizations of profile parameters, mean values were calculated. (from Geringer-Sameth et al., 2015) ([∗] from arxiv:1603.08046v2) NFW profile was used as Dark Matter density profile. Sources are considered as point sources.

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 8 / 17 (Fermi-VERITAS-)HAWC Sensitivity

.-.0. 5 ττ ττ Fermi ττ 10 Years ττ 5 ) 4 1 s 2

5 1 VERITAS - dN/dE TeV/(cm dN/dE 2 1 5

5 Sensitivity E Sensitivity

1 1

11 1 11 1 11 1 2 annihilation values are calculated for Segue 1, < σv >=10−23

HAWC scanned for 1-100 TeV Mχ

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 9 / 17 Systematics on the Limits

Astrophysical systematics HAWC Systematics outer blue: 1.0○ HAWC PSF Signal passing rate inner green: 0.2○ HAWC PSF Measured number of photo-electrons J and D factor integration (PEs) based on simulations angle: ∼0.5○ [purple] – J and D factor Integration angles kept Simulated PMT charge and the constant, but HAWC PSF changes with charge from actual data energy. Uncertainty associated with the – Physical constraint by DM profile yields angular resolution one sided uncertainty — 42% uncertainty for annihilation cross- ∼50% uncertainty [arxiv:1701.01778] section limits — 38% uncertainty for decay lifetime limits

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 10 / 17 Dark Matter Annihilation (Upper) Limits

10 18 10 18

10 20 10 20 ] ] 1 10 22 Preliminary 1 10 22 Preliminary s s 3 3 m m c c [ [

> >

v v + 10 24 bb 10 24 < <

HAWC LeoI CanesVenaticiII HAWC LeoI CanesVenaticiII 10 26 HAWC (w/o TriII) LeoII Sextans 10 26 HAWC (w/o TriII) LeoII Sextans TriangulumII LeoIV UrsaMajorI TriangulumII LeoIV UrsaMajorI Segue1 Hercules UrsaMajorII Segue1 Hercules UrsaMajorII Draco Bootes1 UrsaMinor Draco Bootes1 UrsaMinor ComaB CanesVenaticiI ComaB CanesVenaticiI 10 28 10 28 1.0 10.0 100.0 1.0 10.0 100.0 M [TeV] M [TeV] Ran the analysis for 507 days of HAWC data for five annihilation channels (bb¯, tt¯, WW , ττ, µµ) Combined results were computed for 14 dSph and 14 dSph+TriangulumII Limits are driven by TriangulumII, Segue1 and Coma B ττ is the strongest limit for HAWC [see arXiv:1706.01277]

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 11 / 17 Dark Matter Annihilation (Upper) Limits

10 22 10 22 ] ] 1 1

s 24 s 24

3 10 Preliminary 3 10 Preliminary m m c c [ [

> > v v < <

+ 10 26 bb 10 26 W W

HAWC Veritas Segue1 Magic Segue1 HAWC Sommerfeld DM Magic Segue1 HAWC (w/o TriII) HESS Fermi Combined HAWC (w/o TriII) Veritas Segue1 Fermi Combined Thermal DM Thermal DM 10 28 10 28 1.0 10.0 100.0 1.0 10.0 100.0 M [TeV] M [TeV] Gray band: HAWC systematics, Orange band: Astrophysical systematics HAWC dSph limits are better than VERITAS and HESS, than Fermi after ∼3 TeV. Magic Segue1 limits → negative fluctuation

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 12 / 17 Dark Matter Annihilation (Upper) Limits

10 22 10 22 ] ] 1 1

s 24 s 24

3 10 Preliminary 3 10 Preliminary m m c c [ [

> > v v < <

+ + 10 26 10 26

HAWC Veritas Segue1 Magic Segue1 HAWC Thermal DM Magic Segue1 HAWC (w/o TriII) HESS Fermi Combined HAWC (w/o TriII) Veritas Segue1 Fermi Combined Thermal DM 10 28 10 28 1.0 10.0 100.0 1.0 10.0 100.0 M [TeV] M [TeV] Because of their gamma-ray spectrum, leptonic channel are expected to yield better limits HAWC dSph limits are better after a few TeV M31 limits are comparable and Virgo limits are not good (as expected) M31 is a good source for searching DM annihilation

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 13 / 17 Dark Matter Decay (Lower) Limits

1028 1028

1027 1027

1026 1026

1025 1025 ] ]

s 24 s 24 [ [

10 10

1023 Preliminary 1023 Preliminary + +

1022 HAWC (w/o TriII) LeoI CanesVenaticiII 1022 HAWC (w/ TriII) LeoII Sextans TriangulumII LeoIV UrsaMajorI Combined dSph 1021 Segue1 Hercules UrsaMajorII 1021 M31 Draco Bootes1 UrsaMinor Virgo ComaB CanesVenaticiI Veritas Segue1 1020 1020 100 101 102 100 101 102 M [TeV] M [TeV] Gray band: HAWC systematics, Orange band: Astrophysical systematics Limits are driven by TriangulumII, Segue1 and Coma B (TriangulumII is not so strong, smaller D factor)

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 14 / 17 Dark Matter Decay (Lower) Limits

1028 1028

1027 1027

1026 1026

1025 1025 ] ]

s 24 s 24 [ [ 10 10 HAWC bb (w/o TriII) HAWC tt (w/o TriII) + 1023 Preliminary 1023 PreliminaryHAWC W W (w/o TriII) + + HAWC (w/o TriII) HAWC + (w/o TriII) 22 HAWC (w/o TriII) LeoI CanesVenaticiII 22 10 10 HAWC bb (w/ TriII) HAWC (w/ TriII) LeoII Sextans Veritas Segue1 bb HAWC tt (w/ TriII) TriangulumII LeoIV UrsaMajorI Veritas Segue1 W W + HAWC W W + (w/ TriII) 1021 Segue1 Hercules UrsaMajorII 1021 + + Draco Bootes1 UrsaMinor Veritas Segue1 HAWC (w/ TriII) ComaB CanesVenaticiI Veritas Segue1 + HAWC + (w/ TriII) 1020 1020 100 101 102 100 101 102 M [TeV] M [TeV] HAWC ττ limit is the strongest limit [see arXiv:1706.01277] Virgo is a good source for searching DM decay With the extended source analysis, this will only get better

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 15 / 17 Some other sources

There is also another class of objects: dIrr galaxies - 31 dIrr galaxies in HAWC FOV (5 of them can be considered extended) - Low gamma-ray background - Low baryon-dark matter ratio

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 16 / 17 Summary

Results for 15 dSph were shown (analysis as point sources) Annihilation: Better limits in ττ and µµ channels for Mχ > ∼3 TeV than other experiments Decay: Better limits in all channels compared to other experiments Limits will improve with: including more dSph galaxies more observation time improvements on the analysis techniques and detector

Tolga Yapıcı Dark Matter Searches with HAWC TeVPA 2017, 11 August 2017 17 / 17