Observation of Extended Very High Energy Emission From the Supernova Remnant Ic 443 With Veritas

Acciari, V. A.; Aliu, E.; Arlen, T.; Aune, T.; Bautista, M. A.; Beilicke, M.; Benbow, W.; Bradbury, S. M.; Buckley, J. H.; Bugaev, V.; Butt, Y.; Byrum, K.; Cannon, A.; Çelik, Ö.; Cesarini, A.; Chow, Y. C. K.; Ciupik, L.; Cogan, P.; Colin, P.; Cui, Wei; Daniel, M. K.; Dickherber, R.; Duke, C.; Dwarkadas, Vikram V.; Ergin, T.; Fegan, S. J.; Finley, J. P.; Finnegan, G.; Fortin, P.; Fortson, L.; Furniss, A.; Gall, D.; Gibbs, K.; Gillanders, G. H.; Godambe, S.; Grube, J.; Guénette, R.; Gyuk, G.; Hanna, D.; Hays, E.; Holder, J.; Horan, D.; Hui, C. M.; Humensky, T. B.; Imran, Asif; Kaaret, P.; Karlsson, N.; Kertzman, M.; Kieda, D.; Kildea, J.; Konopelko, A.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Maier, G.; McCann, A.; McCutcheon, M.; Millis, J.; Moriarty, P.; Ong, R. A.; Otte, A. N.; Pandel, D.; Perkins, J. S.; Pohl, M.; Quinn, J.; Ragan, K.; Reyes, Luis; Reynolds, P. T.; Roache, E.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Smith, A. W.; Steele, D.; Swordy, S. P.; Theiling, M.; Toner, J. A.; Valcarcel, L.; Varlotta, A.; Vassiliev, V. V.; Vincent, S.; Wagner, R. G.; Wakely, S. P.; Ward, J. E.; Weekes, T. C.; Weinstein, A. J.R.; Weisgarber, T.; Williams, D. A.; Wissel, S.; Wood, M.; Zitzer, B.

doi:10.1088/0004-637x/698/2/l133

Cited by 136 publications

(85 citation statements)

References 36 publications

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“…The TeV size of IC 443 is from Acciari et al (2009) and W51C is from Krause et al (2011). The TeV sizes of MSH 15−52, HESS J1614−518, HESS J1632−478, and HESS J1837−069 have only been reported with an elliptical 2D Gaussian fit and so the plotted sizes are the geometric mean of the semi-major and semiminor axes.…”

Section: Discussionmentioning

confidence: 99%

SEARCH FOR SPATIALLY EXTENDEDFERMILARGE AREA TELESCOPE SOURCES USING TWO YEARS OF DATA

Landé

Ackermann

Allafort

et al. 2012

ApJ

174

239

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Spatial extension is an important characteristic for correctly associating γ -ray-emitting sources with their counterparts at other wavelengths and for obtaining an unbiased model of their spectra. We present a new method for quantifying the spatial extension of sources detected by the Large Area Telescope (LAT), the primary science instrument on the Fermi Gamma-ray Space Telescope (Fermi). We perform a series of Monte Carlo simulations to validate this tool and calculate the LAT threshold for detecting the spatial extension of sources. We then test all sources in the second Fermi-LAT catalog for extension. We report the detection of seven new spatially extended sources.

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Section: Discussionmentioning

confidence: 99%

SEARCH FOR SPATIALLY EXTENDEDFERMILARGE AREA TELESCOPE SOURCES USING TWO YEARS OF DATA

Landé

Ackermann

Allafort

et al. 2012

ApJ

174

239

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“…W28 is a prominent member of a growing list of SNRs linked to TeV/GeV gamma-ray emission spatially matched with molecular clouds. This list includes HESS J1745−290/SNR G359.1−0.5 (Aharonian et al 2004), HESS J1714−385/CTB 37A (Aharonian et al 2008a), HESS J1923+141/SNR G49.2−0.7 (Feinstein et al 2009) and IC 443 (Albert et al 2008;Acciari et al 2009). All of these SNRs exhibit 1720 MHz OH masers as for W28, and appear to be mature SNRs (age >10 4 yr) whereby any accelerated CRs would have begun to escape into the surrounding interstellar medium.…”

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confidence: 99%

12 mm line survey of the dense molecular gas towards the W28 field TeV gamma-ray sources

Nicholas

Rowell

Burton

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We present 12 mm Mopra observations of dense molecular gas towards the W28 supernova remnant (SNR) field. The focus is on the dense molecular gas towards the TeV gamma‐ray sources detected by the HESS telescopes, which likely trace the cosmic rays from W28 and possibly other sources in the region. Using the NH3 inversion transitions we reveal several dense cores inside the molecular clouds, the majority of which coincide with high‐mass star formation and H ii regions, including the energetic ultracompact H ii region G5.89−0.39. A key exception to this is the cloud north‐east of W28, which is well known to be disrupted as evidenced by clusters of 1720 MHz OH masers and broad CO line emission. Here we detect broad NH3, up to the (9,9) transition, with linewidths up to 16 km s−1. This broad NH3 emission spatially matches well with the TeV source HESS J1801−233 and CO emission, and its velocity dispersion distribution suggests external disruption from the W28 SNR direction. Other lines are detected, such as HC3N and HC5N, H2O masers, and many radio recombination lines, all of which are primarily found towards the southern high‐mass star formation regions. These observations provide a new view on to the internal structures and dynamics of the dense molecular gas towards the W28 SNR field and, in tandem with future higher‐resolution TeV gamma‐ray observations, will offer the chance to probe the transport of cosmic rays into molecular clouds.

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“…The proximity of this line of sight to IC 443, a young SNR known to be interacting with nearby molecular gas, suggests a possible nucleosynthetic origin for the enhancement. The presence of hadronic cosmic rays accelerated by the SNR and their interaction with ambient molecular material was revealed by VERITAS observations of very-high energy γ-ray emission (Acciari et al 2009). HD 43818, however, lies considerably to the north of the γ-ray source and so may not be related.…”

Section: Discussionmentioning

confidence: 99%

Boron abundances in diffuse interstellar clouds

Ritchey¹,

Federman²,

Sheffer³

et al. 2009

Proc. IAU

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Abstract. We present a comprehensive survey of B abundances in diffuse interstellar clouds from HST /STIS observations along 56 Galactic sight lines. Our sample is the result of a complete search of archival STIS data for the B II λ1362 resonance line, with each detection confirmed by the presence of absorption from other dominant ions at the same velocity. The data probe a range of astrophysical environments including both high-density regions of massive star formation as well as low-density paths through the Galactic halo, allowing us to clearly define the trend of B depletion onto interstellar grains as a function of gas density. Many extended sight lines exhibit complex absorption profiles that trace both local gas and gas associated with either the Sagittarius-Carina or Perseus spiral arm. Our analysis indicates a higher B/O ratio in the inner Sagittarius-Carina spiral arm than in the vicinity of the Sun, which may suggest that B production in the current epoch is dominated by a secondary process. The average gas-phase B abundance in the warm diffuse ISM [log (B) = 2.38 ± 0.10] is consistent with the abundances determined for a variety of Galactic disk stars, but is depleted by 60% relative to the solar system value. Our survey also reveals sight lines with enhanced B abundances that potentially trace recent production of 11 B either by cosmic-ray or neutrino-induced spallation. Such sight lines will be key to discerning the relative importance of the two production routes for 11 B synthesis.

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Observation of Extended Very High Energy Emission From the Supernova Remnant Ic 443 With Veritas

Cited by 136 publications

References 36 publications

SEARCH FOR SPATIALLY EXTENDEDFERMILARGE AREA TELESCOPE SOURCES USING TWO YEARS OF DATA

SEARCH FOR SPATIALLY EXTENDEDFERMILARGE AREA TELESCOPE SOURCES USING TWO YEARS OF DATA

12 mm line survey of the dense molecular gas towards the W28 field TeV gamma-ray sources

Boron abundances in diffuse interstellar clouds

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