Brian Humensky for the VERITAS Collaboration December 10, 2009

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1 Brian Humensky for the VERITAS Collaboration December 10, 2009 Univ ersit y of Chicago

2 1ES ES Source Detections in 6 source classes, at least 10 in the Galactic Plane

3 Survey of the Cygnus region in TeV: At < 3% Crab flux Discovery of new source VER J Detection of TeV J Discovery of IC 443 in TeV: Classic SNR / MC interaction system Wonderful laboratory to explore cosmic-ray interaction / diffusion Discovery of SNR G in TeV: Extended TeV source associated with PWN or SNR/MC interaction? Discovery of SNR G in TeV: Young Crab-like PWN Detailed study of Cassiopeia A: Young, nonthermal X-ray SNR VHE spectrum is a power law to 5 TeV Study of gamma-ray binaries: LSI: clear detection only at apastron. Investigation of GeV/TeV differences. HESS J : VERITAS established variability. A new TeV binary system? Cyg X-3: Convincing -ray detections from AGILE, Fermi VERITAS follow-up in spring 2010 Detailed study of Crab Nebula: 5 detection ~ 70 seconds Search for correlation with giant radio pulses (with Green Bank) Stability of TeV flux (with MAGIC) Unidentifieds HESS J and HESS J in the W44 region MGRO J AGILE transient J Northern PWN Survey Limits 3C 58, Geminga, others

4 Effective exposure time [min] VER J Un-biased indication of source population hrs base survey, 56 hrs followup to date VER J : New VERITAS source TeV J : known source, first detected by HEGRA Likely associated: MGRO J , 0FGL J (LAT pulsar) Detection: >5σ at nominal position (no trials) Preliminary Flux Limits above 200 GeV (99% CL, all points in survey below 3σ) <3.0% Crab (point source) <8.5% Crab (0.2 radius extended source) Possible indication that population in Cygnus region differs from inner galaxy HESS survey: of 14 sources in -30 <l< 30, saw 12 sources with fluxes 5% Crab above 200 GeV expect ~2-3 in VERITAS survey see zero

5 In northwest region of Cygni SNR (G ) What exactly is it? PWN? core ~0.5 away from Fermi pulsar Association seems unlikely VERITAS emission does overlap well with radio contours in northwest Shock-cloud interaction? Plenty of CO in southeast, little in northwest Two partial shells in HI, one in northwest (Ladouceur and Pineault 2008, A&A 490, 197) Cloudlets? Enough mass in HI? Speculation: SNR expanded in progenitor s windblown bubble now encountering surrounding swept-up shell VERITAS excess map 1420 MHz CGPS Radio contours PRELIMINARY VERITAS 1σ ellipse LAT PSR J No visible -ray emission to the southeast

6 Troja et al Red: Optical (DSS) Green: CO (Lee et al. 2010, in prep.) Yellow: VERITAS significance (4, 6 ) SNR / MC Interaction + PWN Discovered in GeV by EGRET Now AGILE, Fermi Discovered in TeV in 2007 by VERITAS & MAGIC VERITAS: 8.3, extended emission TeV emission may be CR-induced pion production in cloud associated with the pulsar wind nebula to the south GeV and TeV emission spatially separated? (both extended) Broad-band morphological evolution distinguishes between scenarios (not all PWN) Window into propagation / diffusion of Cosmic Rays in interstellar medium Abdo et al. submitted

7 VERITAS observations resolve TeV emission overlapping the radio shell of G σ detection in 33 hours (6.0 σ post-trials) TeV emission is extended Spans a region Peak is 0.4 (~6 pc) from PSR Overlaps region of high CO density Energy Spectrum power law Index: 2.3 ± 0.3 stat ± 0.3 sys Flux (> 1 TeV) ~ 5% Crab Extrapolation of spectrum is consistent within errors with Milagro point at 35 TeV Excess Map Purple - 12 CO Emission (FCRAO) Yellow star 1AGL J Black Radio (DRAO) Circle FGST Error Box Dot Pulsar Position Acciari et al. 2009, ApJ 703 L6

8 Cousin of the Crab X-ray jet/torus, no thermal shell Age ~ 2900 years E-dot = erg/s Distance ~ 6.2 kpc Location compatible with pulsar Consistent with point source Acciari et al. (2009), in prep. Power-law spectrum: Lu et al (Chandra/ACIS) Index: 2.40 ± 0.24 stat ± 0.3 sys Flux (> 1 TeV) ~ 2.5% Crab L / E-dot ~ 0.15% Similar to other young TeV PWNe, eg G , Kes 75 VHE -rays from freshly injected electrons

9 Young (~330 yr) shell-type SNR Discovered in TeV by HEGRA (232 hrs, 5 ), confirmed by MAGIC (47 hrs, 5.3 ) VERITAS: 22 hr data in 2007, 8.3 Consistent with point source Stage et al Solid: VERITAS Dashed: HEGRA Dotted: MAGIC Chandra Index: 2.61 ± 0.24 stat ± 0.2 sys Flux (> 1 TeV) ~3.5% Crab No sign of a cut-off at high energy. Fermi spectrum connects at lower energy Electrons or hadrons? Acciari et al. 2009, submitted

10 First detected by MAGIC (2006) Intensively observed by VERITAS, Orbital modulation: GeV/TeV anticorrelation Competition between IC and absorption? Spectrum: Fermi cutoff ~6 GeV, VERITAS only 3 since Fermi launch Magnetospheric emission? Stellar weather? Accretion-powered Wind-driven Mirabel (Science 309, 714, 2006) Fermi Fermi MAGIC/VERITAS VERITAS

11 AGILE, Fermi report -ray activity from Cyg X-3 Fermi detects orbital period AGILE detects 4 -ray flares, connects to jet formation VERITAS will follow up in Spring! Abdo et al Science Express VERITAS establishes -ray variability of HESS J Unidentified TeV source in the Galactic plane unresolved! X-ray & radio sources coincident with a Be star (MWC148) Swift: long-term X-ray variability VERITAS, HESS leading MWL campaign to identify source

12 IC 443: Extended and complicated Strong Fermi source: broadband spectral, morphological evolution will be illuminating SNR G /Boomerang: Fermi, VERITAS, MILAGRO Cas A: Best TeV spectrum to date Boon to modelers, especially combined with Fermi spectrum Cygni: Emission not associated with large cloud to south Encountering increasing density to north? LS I : GeV / TeV differences cooling mechanisms? GeV: detected at all phases, peaks at periastron TeV: only clearly detected at apastron HESS J : VERITAS established variability A new TeV binary system? Overall: Lack of strong (>5% Crab) sources (eg, PWNe) Sky survey is addressing this quantitatively

13 Broad-band -ray studies with VERITAS & Fermi Joint analysis (morphology, cross-correlation studies) with Fermi data (funded GI Cycle II proposal) Monitoring of LS I (funded GI Cycle II proposal) Deep observations & detailed studies of sources IC 443, SNR G /Boomerang, Cygni, Cassiopeia A MWL monitoring of known and candidate binary systems Cyg X-3, HESS J , LS I Exploratory observations of candidate TeV emitters Supernova remnants interacting with molecular clouds Nebulae associated with energetic pulsars Follow-up of Fermi galactic sources Unidentifieds use VERITAS angular resolution, lack of diffuse Transients very few so far! response to SGR outbursts now following GRB protocol - fast

14

15 VERITAS Telescope Array VERITAS: Four 12-m diameter atm. Cherenkov telescopes F.L. Whipple Observatory (1.3 km altitude), AZ, USA Staged construction, full sensitivity after Sept Whipple 10m telescope on Mt. Hopkins (2.2 km altitude) 7km away

16 Instrument design: Four 12-m telescopes, 3.5 FoV FLWO, Mt. Hopkins, Az (1268m) Fully operational Sept 2007 Performance: 3-level trigger (250 Hz rate) ~ 800 hrs/yr dark time, ~ 200 hrs/yr moon time Energy threshold ~150 GeV (zenith) Energy resolution ~ % Angular resolution ~ 0.1 7km away Sensitivity: T1 Sep % Crab < 50 hours (before T1 move) 1% Crab < 30 hours (after T1 move) See poster by J. Perkins VERITAS T1 Relocation

17 Discovered by Whipple 10m in 1989 VERITAS: 5 in ~ 1 minute Science Goals Measure/limit extent of TeV emission Stability of Crab emission (w/ MAGIC) Probe correlated variability with Giant Radio Pulses (w/?) Confirm pulsed emission Measure spectrum to high energies Point-source Sensitivity

18 Energy Range: 100 GeV 30 TeV (spectra >150 GeV) Energy Resolution: 15% 20% Effective Area (std. cuts) Crab Rate ~ 40 / min (trigger) Sensitivity: 5% Crab in < 2.5 h 1% Crab in < 50 h Angular Resolution: r 68 < 0.1 o Pointing Accuracy: < 50 Energy Resolution Angular Resolution

19 Currently the most sensitive VHE instrument in the world!

20 1420 MHz: Effelsberg (Kothes et al.) Energetic pulsar + wind nebula discovered in the error box of source 3EG J Age ~ 10,000 years E-dot = erg/s Likely part of the larger SNR G Distance ~ 800 pc (Kothes et al. 2001) Boomerang PWN Fermi: 0FGL J MILAGRO: Extended emission at ~35 TeV

21 Observations made in 2008 resolve TeV emission overlapping the radio shell of G σ detection in 33 hours (6.0 σ post-trials) Excess Map TeV emission is extended Spans a region Peak is 0.4 away from PSR Overlaps with region of high CO density Black Radio (DRAO) Circle FGST Error Box Dot Pulsar Position Purple - 12 CO Emission (FCRAO) Yellow star 1AGL J Acciari et al. 2009, ApJ 703 L6.

22 Energy Spectrum Integrate over 0.32 radius centered on emission peak Well fit by a pure power law Index: 2.3 ± 0.3 stat ± 0.3 sys Flux (> 1 TeV) ~ 5% Crab Extension of spectrum is consistent within errors with Milagro point at 35 TeV Spectrum may favor hadronic origin?

23 Shell interacting with massive cloud Age ~20-30 kyr, 0.75º diameter PWN at southern edge of shell Discovered in GeV by EGRET Now AGILE, Fermi Discovered in TeV in 2007 by MAGIC (5.7 in 29 hrs) by VERITAS (7.1/6.0 pre/post-trials in 15.9 hrs) Green Radio Red Optical Blue X-rays Troja et al. (2006)

24 2-D Gaussian profile fit: Centroid: ± 0.03º stat ± 0.07º sys Extension: σ ~ 0.16º ± 0.03º stat ± 0.04º sys Red: Optical (DSS) Green: CO (Lee et al. 2010, in prep.) Yellow: VERITAS significance (4, 6 ) Total live time: 37.9 hrs. 8.3 σ peak significance pretrials Power-law fit TeV: Index: 2.99 ± 0.38 stat ± 0.3 sys Flux (> 300 GeV) ~ 3.2% Crab TeV emission may be CR-induced pion production in cloud associated with the pulsar wind nebula to the south GeV and TeV emission spatially separated? (both extended) Broad-band morphological evolution distinguishes between scenarios (not all PWN) Window into propagation / diffusion of Cosmic Rays in interstellar medium Acciari et al. 2009, ApJ 698 L133

25 Abdo et al. submitted TeV emission may be CR-induced pion production in cloud associated with the pulsar wind nebula to the south GeV and TeV emission spatially separated? (both extended) Broad-band morphological evolution distinguishes between scenarios (not all PWN) Window into propagation / diffusion of Cosmic Rays in interstellar medium

26 Efficient method of searching for new sources over a large region Un-biased indication of source population Southern hemisphere well-surveyed HESS Galactic plane survey: ~14 sources in initial survey Best limits in northern hemisphere sky : HEGRA s Galactic plane survey -2 < l < 85, flux upper limits: 15% Crab to several Crab Size and choice of region based on VERITAS sensitivity and FOV Material distribution, density of potential TeV γ-ray emitters (SNRs, PWNe, high E-dot pulsars, EGRET unidentified sources...)

27 Effective exposure time [min] Made possible by good off-axis sensitivity Region covered: 67 < l < 82, -1 < b < 4 Available observing period: Apr-Jun, Sep-Nov Effective exposure: ~6 hrs in base survey 112 hours in base survey + 56 hours followup. Prior to Fall

28 VER J VER J New VERITAS source TeV J known source, first detected by HEGRA Likely associated: MGRO J , 0FGL J (LAT pulsar) Detection: >5σ at nominal position (no trials) Partial survey map, generated with standard threshold extended source analysis Includes all data in survey region taken to this point Exposure uneven due to followup (more intensive followup around VER J than around TeV J )

29 Fall 2009 data only Early follow-up candidate Recent (last 2 months) followup treated as an independent search 0.25 radius search region 0.6 wobble, position indicated by earlier data 8.5σ (~7.5σ) pre- (post-) trials in Fall 2009 data alone Position: RA: ± stat Dec: ± stat Extension: 0.16 ± (0.11 ± ) for the major (minor) axis 2-d Gaussian fit to uncorrelated excess map (Fall 2009 data only) Flux ~ few % Crab

30 No hotspots above 5σ post-trials in base survey Preliminary Flux Limits (99% CL, all points in survey below 3σ) <3% Crab above 200 GeV (point source) <8.5% Crab above 200 GeV (0.2 radius extended source) Possible indication that population in Cygnus region differs from inner galaxy HESS survey: out of 14 sources in -30 <l< 30, saw 12 sources with fluxes 5% Crab above 200 GeV expect ~2-3 in this survey Detection of 2 sources with VERITAS survey technique and followup observations Discovery: VER J TeV J2032 Further followup observations in survey region ongoing Prospects for future: Spectra and energy-dependent morphology (VER J , TeV J ) Joint analysis (morphology, cross-correlation studies) with Fermi data

31 Core of VERITAS excess Uchiyama et. al. In 4-10 kev band, pair of faint hard X-ray sources under core (part of C2, Uchiyama et al.) Uchiyama et. al. ApJ, 571: , 2002 Soft X-ray emission belt (1-3 kev) from north to southeast shock interacting with cavity wall of ambient clouds? Suggests hard sources in north are shocked dense cloudlets Nonthermal bremsstrahlung of GeV electrons ASCA X-ray map 4.85 GHz radio contours

32 Detection of 2 sources with VERITAS survey technique and followup observations Discovery: VER J TeV J2032 Further followup observations in survey region ongoing. Prospects for future: Spectra and energy-dependent morphology studies (VER J , TeV J2032). Joint analysis (morphology, cross-correlation studies) with Fermi data in the region.

33 Comparing properties to other young TeV pulsare wind nebulae: Name Edot Dist Lg LX Lg/Edot LX / Edot LX /Lg (erg/s) (kyr) (kpc) (10^34 erg/s) (10^35 erg/s) (%) (%) Crab Nebula G G G Kes Lg: Luminosity in TeV band LX: Luminosity in kev band (Kargaltsev & Pavlov 2008)

34 Results: Unidentified Source HESS J : Only unidentified TeV source that is point-like The Monoceros Loop SNR? Rosette Nebula region Molecular gas, NANTEN Galactic plane survey Green s Catalog position of SNR Radio observations 8.35 GHz kyrs old Distance ~1.5 kpc Interaction with the Rosette nebula? Puehlhofer et al First GLAST Symposium MWC 148

35 Results: Unidentified Source Prob. that VERITAS upper flux limits is consistent with HESS flux is 0.007% (~4 ) Ongoing analysis work: Is there a signal in energy range below 1 TeV? Interpretation: Binary system? Coincident with Be star MWC 148 No companion yet detected; no information on period Variable X-ray emission (Hinton 2009) Acciari et al. 2009, in prep.

36 Results: Unidentified Source Unidentified sources detected in same FoV as the composite SNR W hrs wobbling on W44 position, 4 hrs wobbling on UIDs J possibly associated with newly discovered radio pulsar PSR J W44: UL ~5% Crab J : 4-5 Sigma J : 7-8 Sigma

37 Results: Unidentified Source Transient (E> 100 MeV) AGILE J IGR J EG J Observations (initially under moonlight) triggered by AGILE. 3 Atels (#1492, 1547, 1585) issued on Apr 28, May 27, and Jun by AGILE 7 hour exposure (Apr 29 May 6) 99% upper limit at 2% Crab flux above 300 GeV.

38 Results: Cas A The question of whether or not there is a sufficiently high flux of Galactic nuclear CRs resulting in a steady flux of VHE rays, remains one of the most stimulating scientific questions of ground-based ray astronomy. (Berezhko et al. 2003) The non-thermal X-ray emission predominantly originates from filaments and knots in the reverse-shock region of Cas A (Helder & Vink 2008). The presence of a large flux of high-energy electrons in the reverse-shock region, responsible for the non-thermal radio to X-ray emission, will also produce high-energy - ray emission through non-thermal bremsstrahlung and IC scattering (Atoyan 2006). Based on that leptonic emission, Cas A would appear in VERITAS data as a disk or ringlike source with outer radius 2.5 (Uchiyama & Aharonian 2000). If, on the other hand, the VHE γ -ray emission from Cas A were dominated by 0 decay produced in inelastic collisions of relativistic protons, the location of the particleacceleration site is less constrained by data in other wavebands.

39 Results: Geminga VERITAS Observations: 13.3 hours at high elevation Upper Limit to steady emission(>300 GeV): <2x10-8 γ/m2/s (~1% Crab flux) Upper Limit to pulsed emission(>300 GeV): <1x10-8 γ/m2/s (~0.5% of Crab flux)

40 Results: MGRO J HESS J Needed a test case for Sky Survey extended source search, chose MGRO J /HESS J MGRO unidentified source 80% of Crab Nebula Flux, <2.6 diam. extension at 20 TeV Detected in HESS galactic plane survey 14% Crab flux > 300 GeV Source extension (sys) 0.07 (stat) VERITAS Data taken under aegis of sky survey ~22h of 4-telescope data 4.85σ detection ~ extension position in agreement with HESS J

41 Published papers: 5 LS I data from 2006/7 season, LS I MWL (TeV + X-ray) 2007/8 season IC 443, SNR G /Boomerang HESS J variability Submitted papers: 1 Cassiopeia A Drafted papers: 1 PSR J Papers in preparation: 4 Sky Survey, Cygni, TEV J W44 / HESS J / HESS J region Papers in development: 2 Supernova Remnant upper limits Pulsar Wind Nebula upper limits

42 Merger of several interrelated science groups: Sky Survey SNRs & PWNe Compact Objects Unidentified Sources Telecons ~ monthly to discuss observing proposals, results, papers, Two Key Science Projects: Survey of Cygnus Region Studies of Supernova Remnants and Pulsar Wind Nebulae

43 IC 443 SNR G / Boomerang SNR G / PSR J Cassiopeia A

44

45 Summary VERITAS is operating very well (> 95% uptime) with two+ good years of data in hand. Many new results, including: Discovery of -ray emission from starburst galaxy M82. New information on origins of cosmic rays. Stringent limits from Galactic plane survey. Detection of new TeV source near Cygni SNR, VER J Detection of 2 new PWN/SNR: G , G Detailed studies of SNRs: IC 443 and Cas-A. VERITAS Upgrade will significantly improve sensitivity. T1 Relocation already has! Broad-band studies (GeV TeV) underway much more to come.

46 IC 443: Extended and complicated Hints of energy-dependent morphology in TeV band Strong Fermi source: broadband spectral, morphological evolution will be illuminating Cas A: Best TeV spectrum to date Boon to modelers Cygni: Emission not associated with large cloud to south Cloudlets to the north? LS I : GeV / TeV differences cooling mechanisms? GeV: detected at all phases, peaks at periastron TeV: only clearly detected at apastron Rapid X-ray variability (doubling times short as 2 seconds!) General: Lack of strong (>5% Crab) sources (eg, PWNe) Sky survey is addressing this quantitatively

47 Many of our sources show significant extent IC 443, Boomerang, MGRO J1908 This matches HESS experience: Almost all Galactic sources (minus Crab, Cas A, binaries) are extended Observing: Default 0.5º wobble may not be appropriate for Galactic sources where extent is a priori unknown Issue both for detection (potentially) and spectra (definitely) Larger wobbles? Mini surveys? Moonlight is fruitful for Galactic sources PSR J1930, LS I Analysis: More effort needed on extended sources Background models for detection, spectra Handling of bright stars, angular resolution Likelihood methods for extended sources?

48 Young (~330 yr), well studied shell-type SNR Distance ~3.4 kpc 5-arcmin diameter Comparable to TeV PSF Discovered in TeV by HEGRA (232 hrs, 5 ), confirmed by MAGIC (47 hrs, 5.3 ) Stage et al (Chandra, 7.3 by 6.4 )

49 VERITAS: 22 hr data in 2007, 8.3 Consistent with point source To be replaced by spectrum including Fermi points Solid: VERITAS Dashed: HEGRA Dotted: MAGIC Index: 2.61 ± 0.24 stat ± 0.2 sys Flux (> 1 TeV) ~3.5% Crab No sign of a cut-off at high energy. Fermi spectrum connects at lower energy Electrons or hadrons? Acciari et al. 2009, submitted

50 Cousin of the Crab X-ray jet/torus, no thermal shell Age ~ 2900 years E-dot = erg/s Distance ~ 6.2 kpc Lu et al (Chandra/ACIS)

51 Hint of signal in 2007 moonlight data. 2008/09 follow-up yields a 7-σ detection in 31 hours Location compatible with pulsar Consistent with point source. Acciari et al. (2009), in prep.

52 Chandra X-ray image Cassiopeia A is a young SNR, ~ 320 yrs old X-ray synchrotron (like SN 1006) First SNR detected in TeV gamma rays! By HEGRA in 2001 since detected by VERITAS and MAGIC as well Does it accelerate ions, or just electrons? m m m m ~ 5 arcmin

53 Introduction Survey of the Cygnus Region Detections of SNRs and PWNe -ray Binaries Summary Unidentifieds HESS J and HESS J in the W44 region MGRO J AGILE transient J Northern PWN Survey Limits 3C 58, Geminga, others

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