15 years of Dark Matter searches with MAGIC Michele Doro* - - PowerPoint PPT Presentation

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15 years of Dark Matter searches with MAGIC Michele Doro* - - PowerPoint PPT Presentation

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15 years of Dark Matter searches with MAGIC Michele Doro* *University and INFN Padova michele.doro@pd.infn.it J. Aleksic, J. A. Barrio, A. Biland, A. Dominguez, D. Elsaesser, M. Gaug, P. Giammaria, S. Lombardi, C. Maggio, M. Martinez, D.

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15 years of Dark Matter searches with MAGIC

Michele Doro*

*University and INFN Padova michele.doro@pd.infn.it

  • J. Aleksic, J. A. Barrio, A. Biland, A. Dominguez, D. Elsaesser, M. Gaug, P. Giammaria, S.

Lombardi, C. Maggio, M. Martinez, D. Nieto, D. Ninci, S. Paiano, J. Palacio, F. Prada, M. Persic, J. Rico, M. Rissi, M. A. Sanchez-Conde, K. Satalecka, S. Stark, G. Vanzo, M. Vazquez, F. Zandanel

M . Doro - 15 years of dark m a2er searches w ith M AGIC - La Palm a 2018 1

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Thanks!

2

HAL(O)

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CACTUS claim

  • CACTUS (Converted Atmospheric

Cherenkov Telescope Using Solar-2) was a ACT located in California.

  • It was originally a solar power plant called

Solar Two, converted to an observatory in 2001, installing a 6 meter secondary that imaged the field onto an array of 80 PMTs.

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BergstromHooper 2015

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Dwarf Spheroidal Galaxies (dSphs)

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12 years ago

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ShallowDM profile Peaked DM profile

àMAGICß GLAST

40 hours of observation time,

  • ne year of observation time

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Classical and Ultra-faint dwarf spheroidal galaxies

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Belokurov+ (SDSS) Astrophys.J. 654 (2007) 897-906

Half-light radius Brightness

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Sloan Digital Sky Survey

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Excitement for the ultra-faints

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Strigari+ Nature 454 (2008) 1096-1097

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Crazy for dSphs

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MD, NIM A 742 (2014)

  • All instruments

launched in the search!...but investing few hours

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Draco & Willman 1 with MAGIC

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800 years

7.8 h of data! Battaglia Eur.Phys.J.C33:273-296,2004 m0 m1/2 13.7 h of data!

Draco

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Then Segue1 came

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Segue 1 performed by the MAGIC-I ground-based gamma-ray telescope between 2008 and 2009 for a total

  • f 43.2 hours.

Custom scan

  • fthe

parameter space with DarkSusy within mSugra

M . Doro - 15 years of dark m atter searches w ith M AGIC - La Palm a 2018

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2009: Two (MAGIC) is better than one

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  • 4-fold improvement in sensitivity

↑16 times less needed observation time!

  • 10-fold at lowest energies
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Some expectations for M-stereo: Draco and Willman1

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Bringmann, MD, Fornasa JCAP01(2009)016

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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

How many gamma-rays from DM annihilation/decay?

  • HunOng the

highest J- factor

  • Huge

uncertain;es in the par;cle physics

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DM particle – yes, but which one?

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?

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Segue1 with HiFi system

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Segue 1 with the MAGIC Telescopes, carried out between 2011 and 2013. With almost 160 hours

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Annihilating and decaying dark matter

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Annihilation cross-section Decay lifetime

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Segue 1 – stereo results

  • MAGIC decided to

perform the longest exposure

  • n a single dSph:

Segue 1

  • 160 hours of good-

quality data between 2011 and 2013.

  • 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

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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

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Aleksic, Rico, Martinez JCAP 1210 (2012) 032

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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

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«Gather them all»

  • A project between MAGIC,

VERITAS, HESS and Fermi started to gather them all

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

  • Great expecta>ons!

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

Not only dSphs

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

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Adapted by H. Zechlin

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

Decay DM case

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ANNIHILATING DARK MATTER DECAYING DARK MATTER Signal strength DECAY

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2018: another dSph in the portfolio: Ursa Maior 2

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MAGIC Observation of Perseus Galaxy Cluster

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TODAY on ARXIV 1806.11063

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It all started with cluster

  • F. Zwicky, while examining the Coma galaxy cluster in 1933, was the first

to use the virial theorem to infer the existence of unseen matter, which he referred to as dunkle Materie 'dark matter’. 2 "# = −& à ' ( =

)* +, ,

  • He calculated the gravitational mass of the galaxies within the cluster

and obtained a value at least 400 times greater than expected from their luminosity

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Fritz Zwicky (1898, 1974) The technique was refined by Vera Cooper (Rubin) for galaxies in the ‘60s

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A long campaign

  • Consider duty cycle is roughly 1000h/year

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A very fruitful campaign

  • MAGIC campaign on Perseus CG proved to

be very frui:ul: – the strongest limits on Cosmic Ray (CR) accelera8on in the core of the cluster and on the CR to thermal pressure (Aleksic ́ et al., 2010a, 2012c); – the radio-galaxy NGC 1275, at the center of the cluster, was clearly detected and modelled (Aleksic ́ et al., 2012d, 2014b); and – the peculiar radio-galaxy IC 310, located at 0.6 deg from the Perseus CG center, was detected and provided important evidences related to the acceleraLon of CRs close to black holes (Aleksic ́ et al., 2010b, 2014a,d).

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  • J. Aleksic ́ et al. Astrophys. J., 710:634–647, 2010a.
  • J. Aleksic ́ et al. Astrophys. J., 723:L207, 2010b
  • J. Aleksic ́ et al. Astron. Astrophys., 541:A99, 2012c.
  • J. Aleksic ́ et al. Astron. Astrophys., 539:L2, 2012d.
  • J. Aleksic ́ et al. Astron. Astrophys., 563: A91, 2014a.
  • J. Aleksic ́ et al. Astron. Astrophys., 564:A5, 2014b.
  • J. Aleksic ́ et al. Science, 346:1080–1084, 2014d

See backup slides See Paneque talk

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Complex observing region

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  • Two radio galaxies: NGC1275

and IC310

  • Variability of these sources
  • Extension of DM signal
  • Signal leakeage into

background control region

  • Development of a specific

tailored MC to estimate IRFs properly (J. Palacio Phd 2018)

  • DECAYING DARK MATTER CASE
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Dark matter profile

  • We follow the prescrip/on in Sanchez-Conde et al. (2011)
  • We use 30% systema;cs on mass es;ma;on for Perseus CG (Reiprich

and Boehringer, 2000; Chen et al., 2007)

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Results

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Lines ↓ Continuumà

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MAGIC results put into context

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Why should be using IACT time for DM?

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0/ DM is gravita/onal!

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1/ We do expect gamma-rays

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2/ Dark Matter identification

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3/ Universality of Dark Matter Spectra

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4/ Complementarity

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  • M. Cahill-Rawley 1411.3353

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Are we close or far?

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MAGIC on 10xSegue1 in 500h

Leane+ arXiv:1805.10305,

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More visible dSphs coming

New instruments are discovering new dSphs: some very promising. Expect results from MAGIC!

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We need accurate J-factors (more than precise)

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Chiappo+ 2012

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Dark subhaloes?

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Savala+ MNRAS 457 (2016)

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Conclusions

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MAGIC

  • 3 orders of magnitude

from first to latest limits!

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Can be a long journey to discovery

  • The bus that Bruno

Rossi set-up to carry the experimental equipment to measure Cosmic Rays to the summit of Mount Evans in Colorado (4,348 m).

  • He brought his family

too!

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What about n, h, GW ?

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CTA is happening right here: high expecta2ons for DM searches

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Before their light is switched off Use MAGIC VERITAS and HESS for dSph deep field?

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Happy 15th Birthday!