Search of dark matter in dwarf galaxies with ground-based gamma-ray - - PowerPoint PPT Presentation

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Search of dark matter in dwarf galaxies with ground-based gamma-ray - - PowerPoint PPT Presentation

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Search of dark matter in dwarf galaxies with ground-based gamma-ray detectors Michele Doro University and INFN Padova michele.doro@unipd.it Michele Doro - Halo Workshop - Madrid 2018 1 https://www.darkmatterwines.com/ 2 Michele Doro - Halo

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Search of dark matter in dwarf galaxies with ground-based gamma-ray detectors

Michele Doro

University and INFN Padova michele.doro@unipd.it

Michele Doro - Halo Workshop - Madrid 2018

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https://www.darkmatterwines.com/

Michele Doro - Halo Workshop - Madrid 2018

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Tasting dark matter with gamma rays

Michele Doro - Halo Workshop - Madrid 2018

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0/ DM is there!

Michele Doro - Halo Workshop - Madrid 2018

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1/ We do expect gamma-rays

Michele Doro - Halo Workshop - Madrid 2018 5

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2/ Dark Matter mass (cutoff position) & Dark matter branching ratios (spectral shape)

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Bringmann, Doro, Fornasa JCAP01(2009)016

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3/ Universality of Dark Matter Spectra

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Astrophysical factor: Particle Physics factor: Annihilation: Decay:

Large uncertainties from Fund. Phys. No target dependences (straightforward stacking analysis) Large uncertainties from DM profiles (robust limits from less uncertain targets) dec

1 tc

  • S. Lombardi (INAF-OAR & ASDC), Dark Side of the Universe 2016, Bergen, 25-29 July 2016

What influences the flux on Earth

  • Hunting the

highest J- factor

  • Left with huge

uncertainties in the particle physics

Michele Doro - Halo Workshop - Madrid 2018 8

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  • S. Lombardi (INAF-OAR & ASDC), Dark Side of the Universe 2016, Bergen, 25-29 July 2016

Where to look

vGalactic halo and the halo around

+ Highest J-factor

  • Strong Astrophysical contamination
  • Huge uncertaintiy in core\cusp

− “wrong” hemisphere for MAGIC)

v Galaxy Clusters

+ Huge amount of DM but far distance à moderate/low J-factor − High astropysocal contamination

  • Large uncertainties in baryon feedback and

substructure contributions − Extended

v Dwarf Galaxies

+ DM dominated (high M/L ratios) and Free from astroph. bkg + Less uncertainties on J-factors

  • Low J-factor

v Dark Clumps?

+ Free from astroph. bkg + Nearby and numerous − How to know where they are? − Bright enough?

v DM anisotropies

+ In principle possible with IACTs although challenging

Michele Doro - Halo Workshop - Madrid 2018 9

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  • S. Lombardi (INAF-OAR & ASDC), Dark Side of the Universe 2016, Bergen, 25-29 July 2016

If you need to point, where to point?

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ANNIHILATING DARK MATTER DECAYING DARK MATTER Signal strength DECAY

Michele Doro - Halo Workshop - Madrid 2018

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What was accomplished with gamma rays

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Techniques

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Compton (in space) 10 MeVà Pair-production (in space) 100 MeV—100 GeV Cherenkov (ground) 10 GeV—100 TeV Shower front (ground) 1 TeV—100TeV+

Bad angular pos.

Michele Doro - Halo Workshop - Madrid 2018 Modified from: Hofmann 2012

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A question of calorimeters

  • Calorimeter manmade:

– Water Cherenkov: HAWC, LATTES, MILAGRO – Satellite pair-conversion instruments: Agile, Fermi-LAT

  • Calorimeter provided by nature:

– Imaging experiment: IACT: MAGIC, HESS, VERITAS, CTA,

  • Imaging:

– Showers create images in the camera whence the shower is totally contained – The image is the event – Stereoscopy is very important

  • M. Doro - Exotic needles in the gamma-ray haystack - RICAP 2016

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Comparing experiments

Sensitivity is not the only thing that matters

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Plot from de Angelis, Mallamaci https://arxiv.org/abs/1611.02232

Michele Doro - Halo Workshop - Madrid 2018

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Ingredients to discovery

  • Compton: 10 deg
  • Lat/MeV: >1 deg
  • Lat/GeV: 0.5 deg
  • IACT: <0.1 deg
  • EAS: 0.5-1deg

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  • Compton: 20%
  • Lat/MeV: 20%
  • Lat/GeV: 10%
  • IACT: 10-20%
  • EAS: 100%
  • Similar information than

sensitivity for non-transient sources

  • Do not take constant eff.

area And also FOV & Duty cycle

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Steady or not

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IACTs (FOV <5x5)

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HESS, MAGIC and VERITAS (in 2012)

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Happy 15° birthday MAGIC Florian Goebel telescopes!

First light in October 2003

  • M. Doro - MAGIC - CRIS 2018

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IACTs: tested several target classes

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(oudated) MD, NIM A 742 (2014)

Michele Doro - Halo Workshop - Madrid 2018

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Dark matter searches: 1000h+ in a decade

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About 1000 h in a decade ç

MD XXV ECRS 2016 Proceedings

Michele Doro - Halo Workshop - Madrid 2018

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Observe them all

  • Few hourà more than

hundred hours

  • Classical à SDSS-ultra-

faint à DES-ultra-faint

Michele Doro - Halo Workshop - Madrid 2018 21

UNDISCLOSED

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Segue 1 Deep Scan with MAGIC stereo

  • Longest

exposure on a single dSph: Segue 1: 160 hours.

  • Optimized

statistical treatment allowed performance boost

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  • Strongest

constraints above few hundreds GeV according to channel

  • Results made

into the PDG

See Aleksic+ JCAP 1210 (2012) 032

Michele Doro - Halo Workshop - Madrid 2018

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Segue stereo stat treatment

  • In all DM searches, we try to

measure the same universal parameter, e.g. <!"> through gamma-ray flux:

  • Different observations of

different targets differ in the astrophysical or J-factor

  • Aim: combine measurements of

<!"> from different targets and instruments

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The likelihood was prepared so that results from different experiments could be combined The instrument response functions do not need to be combined, but can be used on individual factor of the likelihoodàGREAT ADVANTAGE RESULTS FROM DIFFERENT INSTRUMENTS AND DIFFERENT TARGETS CAN BE NOW COMBINED TO IMPROVE SENSITIVITY

Michele Doro - Halo Workshop - Madrid 2018

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MAGIC + Fermi combined

  • MAGIC: Segue 1 (158 h) and

Fermi-LAT: 15 dwarfs (6 years, Pass8)

  • Effective combination (2x

stronger constraints) in the range 300-500 GeV

24 JCAP 02 (2016) 039 Michele Doro - Halo Workshop - Madrid 2018

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«Gather them all»

  • A project between MAGIC,

VERITAS, HESS and Fermi started to combine them all

– 300+ h MAGIC – 300+ h VERITAS – 100+ h HESS – Fermi-dSph

  • Great expectations!

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J.R.R. Tolkien's epigraph to The Lord of the Rings "Three Rings for the Elven-kings under the sky, Seven for the Dwarf-lords in their halls of stone, Nine for Mortal Men doomed to die, One for the Dark Lord on his dark throne. In the Land of Mordor where the Shadows lie. One Ring to rule them all, One Ring to find them, One Ring to bring them all and in the darkness bind them."—

J.R.R. Tolkien’s abstract of MNRAM "Three DSPHS for the HESS under the sky, Seven for VERITAS in its halls of stone, Nine for MAGIC doomed to rise. One for the Dark MATTER Lord

  • n his dark MATTER throne. In

the Land of FERMI where the GAMMAs lie. One LKL to rule them all, One LKL to find them, One LKL to bring them all and in the darkness PUBLISH them."—

Michele Doro - Halo Workshop - Madrid 2018

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One or many?

  • If we find one dSph with

J=10x J_Segue, in 500h we barely start to enter the holy region

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MD XXV ECRS 2016 Proceedings Leane+ 2018

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MAGIC program

New instruments are discovering new dSphs: some very promising. Expect follow-up from MAGIC!

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Huston: we have a problem. The case of Tri2

  • In 2016, MAGIC

had strong reasons to believe Triangulum 2 was the most DM dominated dSph

  • Discussion whether

to observe it

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Hayashi

  • The usual

“among analyzed dSphs, Triangulum 2 and Ursa Major II ultra faint dwarf galaxies are the most promising but large uncertain targets for dark matter annihilation while Draco classical dSph is the most robust and detectable target for dark matter decay.”

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Is Tri2-large J-factor real?

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Hutten+ 1606.04898 cumulative distribution of all known dSph galaxy objects Calore+ 1611.03503

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Our own checks

Own checks with Clumpy to investigate J-factor

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The killer paper

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Despite that

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DES, LSST, GAIA

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Remove foreground star Advanced spectroscopy

What more?

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Do we know dSph?

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Eline Tolstoy, BAM workshop, Barolo 2017

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We need accurate J-factors (not precise)

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Chiappo+ 2012

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  • Dark clumps should exist!
  • H. Zechlin:

Another dark way

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Dark clumps in plain sight

« […]we find a significant preference (TS = 40) for describing 47 Tuc’s spectrum with a two source population model, consisting of an ensemble of MSPs and annihilating dark matter (DM) with an enhanced density around the IMBH, when compared to an MSP-only explanation. The best-fit DM mass of 34 GeV.»

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Lines searches with dSphs

  • Limits were produced for narrow-band emissions (smoking guns) with

160 hours of Segue1

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MAGIC, JCAP 02 (2014) 008

Michele Doro - Halo Workshop - Madrid 2018

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Shower front detectors

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if m=10 TeV HAWC (left) à 2015 LHAASO (right) à in construction (2019?)

Michele Doro - Halo Workshop - Madrid 2018

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Particle Shower Detectors @ Southern Hemisphere

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arXiv:1607.03051

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HAWC

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When can we toss for DM discovery? A look ahead: CTA

Michele Doro - Halo Workshop - Madrid 2018

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44The Cherenkov Telescope Array Michele Doro - Halo Workshop - Madrid 2018

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Performance limitations in IACTs

Michele Doro - Halo Workshop - Madrid 2018 45 From Hofmann 2012

You can use some brute force You need to use your brain You are not (a) God

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Dark Matter on CTA television

Featuring:

Improved sensitivity Better energy and angular resolution Two hemispheres for hunt Open observatory

Plot:

500h on the GC region (first year(s)) 100h/dSph/year? LMC Can CTA make a change?

MIGUEL ANGEL SANCHEZ CONDE CTA DM WORKING GROUP

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Yes!

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  • However, strong

competition with astro- targets!

  • Need robust (and high)

J-factors!

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CTA with in survey mode (divergent pointing)

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Dark Matter Array

Did this make sense?

51 Michele Doro - Halo Workshop - Madrid 2018 Phys.Rev.D83:045024,2011

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Before their death… Use MAGIC VERITAS and HESS for dSph deep field?

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CONCLUSIONS

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Our heads in the clouds

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?

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Where to look?

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Complementarity

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  • M. Cahill-Rawley 1411.3353

Michele Doro - Halo Workshop - Madrid 2018

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Are we close or far?

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MD XXV ECRS 2016 Proceedings

dSph with J=10x J_Segue, in 500h

Leane+ arXiv:1805.10305,

Michele Doro - Halo Workshop - Madrid 2018

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Conclusions

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Gamma rays are a powerful probe, but so far nothing Still one of best, maybe unique, messenger toward dark matter discovery and identification We need to orientate this future, with CTA and other instruments

Thanks

Michele Doro - Halo Workshop - Madrid 2018

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Announcements

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  • Starting from this year external

scientists can apply for

  • bservation time with MAGIC.

Deadline for the call is set on November 2017: https:/ /magic.mpp.mpg.de/outsider s/magicop/

  • Some MAGIC groups accepts

PhD “affiliation”: If you interested in MAGIC data, phd can JOIN OUR SCIENCE PROGRAM without fees

Michele Doro - Halo Workshop - Madrid 2018