Discovery of Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Kesteven 79

Kuriki, Mika; Sano, Hidetoshi; Kuno, Nario; Seta, Masumichi; Yamane, Yumiko; Inaba, T.; Nagaya, Takashi; Okawa, Kazuki; Tsutsumi, Daichi; Hattori, Yusuke; Kohno, Mikito; Fujita, Shinji; Nishimura, Atsushi; Ohama, Akio; Matsuo, Mitsuhiro; Tsuda, Yuichi; Torii, Kazufumi; Minamidani, Tetsuhiro; Umemoto, Tomofumi; Rowell, G.; Bamba, Aya; Tachihara, Kengo; Fukui, Y.

doi:10.3847/1538-4357/aad7be

Cited by 29 publications

(23 citation statements)

References 59 publications

(75 reference statements)

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“…Next, we argue that Hi clouds at V LSR ∼117.1-122.5 km s −1 and the molecular clouds C and D are also asso-ciated with the SNR in addition to clouds A, B, F, and G. The hollowed out structure in the position-velocity diagram of Hi is likely an expanding gas motion originated from stellar winds from a massive progenitor. The expanding velocity ∆V is estimated to be ∼3 km s −1 , which is roughly consistent with the Galactic CC SNR Kesteven 79 (∆V ∼4 km s −1 ; Kuriki et al 2018). In fact, the metal abundances of the SNR favor the CC explosion (see Section 4.1), which can create a windblown bubble.…”

Section: Molecular and Atomic Clouds Associated With The Smc Snr Rx Jsupporting

confidence: 69%

“…The hadronic γ-ray spectrum, F (ε), therefore, rises steeply below ∼200 MeV in the ε 2 F (ε) representation. The other is probing the good spatial correspondence between the γ-rays and interstellar protons, which is an essential signature of the hadronic γ-rays (Fukui et al 2003(Fukui et al , 2017Fukui 2013;Aharonian et al 1994Aharonian et al , 2008Hayakawa et al 2012;Yoshiike et al 2013;Maxted et al 2012Maxted et al , 2013aMaxted et al ,b, 2018aFukuda et al 2014;Lau et al 2017Lau et al , 2019de Wilt et al 2017;Sano et al 2017cSano et al , 2019bKuriki et al 2018). For RX J0046.5−7308, the eight molecular clouds have the potential to be detected by TeV γ-rays using the Cherenkov Telescope Array with deep exposure.…”

Section: Prospects For γ-Ray Observationsmentioning

confidence: 99%

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Discovery of Shocked Molecular Clouds Associated with the Shell-type Supernova Remnant RX J0046.5−7308 in the Small Magellanic Cloud

Sano

Matsumura

Yamane

et al. 2019

ApJ

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RX J0046.5−7308 is a shell-type supernova remnant (SNR) in the Small Magellanic Cloud (SMC). We carried out new 12 CO(J = 1-0, 3-2) observations toward the SNR using Mopra and the Atacama Submillimeter Telescope Experiment. We found eight molecular clouds (A-H) along the X-ray shell of the SNR. The typical cloud size and mass are ∼10-15 pc and ∼1000-3000 M ⊙ , respectively. The X-ray shell is slightly deformed and has the brightest peak in the southwestern shell where two molecular clouds A and B are located. The four molecular clouds A, B, F, and G have high intensity ratios of 12 CO(J = 3-2) / 12 CO(J = 1-0) > 1.2, which are not attributable to any identified internal infrared sources or high-mass stars. The Hi cavity and its expanding motion are found toward the SNR, which are likely created by strong stellar winds from a massive progenitor. We suggest that the molecular clouds A-D, F, and G, and Hi clouds within the wind-blown cavity at V LSR = 117.1-122.5 km s −1 are associated with the SNR. The X-ray spectroscopy reveals the dynamical age of 26000 +1000 −2000yr and the progenitor mass of 30 M ⊙ , which is also consistent with the proposed scenario. We determine physical conditions of the giant molecular cloud LIRS 36A using the large velocity gradient analysis with archival datasets of the Atacama Large Millimeter/submillimeter Array; the kinematic temperature is 72 +50 −37 K and the number density of molecular hydrogen is 1500 +600 −300 cm −3 . The next generation of γ-ray observations will allow us to study the pion-decay γ-rays from the molecular clouds in the SMC SNR.

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Section: Molecular and Atomic Clouds Associated With The Smc Snr Rx Jsupporting

confidence: 69%

Section: Prospects For γ-Ray Observationsmentioning

confidence: 99%

Discovery of Shocked Molecular Clouds Associated with the Shell-type Supernova Remnant RX J0046.5−7308 in the Small Magellanic Cloud

Sano

Matsumura

Yamane

et al. 2019

ApJ

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“…This means that the expanding gas motion was possibly created by stellar winds or accretion winds from the progenitor system of the SNR (e.g. Sano et al 2017bSano et al , 2018Kuriki et al 2018), which gives alternative support for the physical association between the SNR shocks and the ISM. The minimum intensity spot corresponding to a geometric center of the expanding shell is l ∼ 159.…”

Section: Co and H I Analysis Resultsmentioning

confidence: 99%

Discovery of recombining plasma inside the extended gamma-ray supernova remnant HB9

Sezer

Ergin

Yamazaki

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present the results from the Suzaku X-ray Imaging Spectrometer observation of the mixed-morphology supernova remnant (SNR) HB9 (G160.9+2.6). We discovered recombining plasma (RP) in the western Suzaku observation region and the spectra here are well described by a model having collisional ionization equilibrium (CIE) and RP components. On the other hand, the X-ray spectra from the eastern Suzaku observation region are best reproduced by the CIE and non-equilibrium ionization model. We discuss possible scenarios to explain the origin of the RP emission based on the observational properties and concluded that the rarefaction scenario is a possible explanation for the existence of RP. In addition, the gamma-ray emission morphology and spectrum within the energy range of 0.2−300 GeV are investigated using ∼10 years of data from the Fermi Large Area Telescope (LAT). The gamma-ray morphology of HB9 is best described by the spatial template of radio continuum emission. The spectrum is well-fit to a log-parabola function and its detection significance was found to be ∼25σ. Moreover, a new gamma-ray point source located just outside the south-east region of the SNR's shell was detected with a significance of ∼6σ. We also investigated the archival H i and CO data and detected an expanding shell structure in the velocity range of −10.5 and +1.8 km s −1 that is coinciding with a region of gamma-ray enhancement at the southern rim of the HB9 shell.

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“…The distance of Kes 79 is not very well constrained. One of the most recent estimates, inferred from H i absorption, yields a distance of 3.5 kpc (Ranasinghe & Leahy 2018), whereas CO observations (Kuriki et al 2018) suggest a distance of 5.5 kpc. The age of Kes 79 is estimated via detailed X-ray spectroscopy to lie between 4.4 and 6.7 kyr (Zhou et al 2016).…”

Section: Kes 79mentioning

confidence: 99%

A kinematic study of central compact objects and their host supernova remnants

Mayer

Becker²

2021

A&A

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Context. Central compact objects (CCOs) are a peculiar class of neutron stars, primarily encountered close to the center of young supernova remnants (SNRs) and characterized by thermal X-ray emission. Measurements of their proper motion and the expansion of the parent SNR are powerful tools for constraining explosion kinematics and the age of the system. Aims. Our goal is to perform a systematic study of the proper motion of all known CCOs with appropriate data available. From this, we hope to obtain constraints on the violent kick acting on the neutron star during the supernova explosion and infer the exact site of the explosion within the SNR. In addition, we aim to measure the expansion of three SNRs within our sample to obtain a direct handle on their kinematics and age. Methods. We analyze multiple archival Chandra data sets that consist of HRC and ACIS observations separated by temporal baselines of between 8 and 15 years. We achieve accurate source positions by fitting the imaging data with ray-tracing models of the Chandra point spread function. In order to correct for Chandra’s systematic astrometric uncertainties, we establish a reference frame using X-ray-detected sources in Gaia DR2 to provide accurate proper motion estimates for our target CCOs. Complementarily, we use our coaligned data sets to trace the expansion of three SNRs by directly measuring the spatial offset of various filaments and ejecta clumps between different epochs. Results. In total, we present new proper motion measurements for six CCOs. Within our sample, we do not find any indication of a hypervelocity object, and we determine comparatively tight upper limits (< 230 km s−1) on the transverse velocities of the CCOs in G330.2+1.0 and RX J1713.7−3946. We tentatively identify direct signatures of expansion for the SNRs G15.9+0.2 and Kes 79, at an estimated significance of 2.5σ and 2σ, respectively. Moreover, we confirm recently reported results, measuring the rapid expansion of G350.1−0.3 at almost 6000 km s−1, which places its maximal age at 600 − 700 years, making this object one of the youngest Galactic core-collapse SNRs. The observed expansion, combined with the proper motion of its CCO, which is much slower than previously predicted, implies the need for a very inhomogeneous circumstellar medium to explain the highly asymmetric appearance of the SNR. Finally, for the SNR RX J1713.7−3946, we combine previously published expansion measurements with our measurement of the CCO’s proper motion to obtain a constraining upper limit of 1700 years on the system’s age.

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Discovery of Molecular and Atomic Clouds Associated with the Gamma-Ray Supernova Remnant Kesteven 79

Cited by 29 publications

References 59 publications

Discovery of Shocked Molecular Clouds Associated with the Shell-type Supernova Remnant RX J0046.5−7308 in the Small Magellanic Cloud

Discovery of Shocked Molecular Clouds Associated with the Shell-type Supernova Remnant RX J0046.5−7308 in the Small Magellanic Cloud

Discovery of recombining plasma inside the extended gamma-ray supernova remnant HB9

A kinematic study of central compact objects and their host supernova remnants

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