Cosmic Origins Spectrograph Observations of the Chemical Composition of SNR LMC N132d

France, Kevin; Beasley, Matthew; Keeney, Brian A.; Danforth, Charles W.; Froning, Cynthia S.; Green, James C.; Shull, J. M.

doi:10.1088/0004-637x/707/1/l27

Cited by 32 publications

(21 citation statements)

References 23 publications

(33 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…While the COS resolution of a point source is ∼20 km s −1 , a fully filled aperture has a resolution approaching 200 km s −1 (France et al 2009). During the fitting process we convolve the Milky Way fits with a Gaussian and fit for a FWHM to account for the spectral resolution.…”

Section: Milky Way Line Fittingmentioning

confidence: 99%

Scaling Relations Between Warm Galactic Outflows and Their Host Galaxies

Chisholm¹,

Tremonti²,

Leitherer

et al. 2015

ApJ

157

211

View full text Add to dashboard Cite

We report on a sample of 48 nearby, star-forming galaxies observed with the Cosmic Origin Spectrograph on the Hubble Space Telescope. We measure the kinematics of warm gas in galactic outflows using a combination of four Si II absorption lines. We use multi-wavelength ancillary data to estimate stellar masses (M * ), star formation rates (SFR), circular velocities (v circ ), and morphologies. The galaxies cover four orders of magnitude in M * and SFR, and sample a wide range of morphologies from starbursting mergers to normal star-forming galaxies. We derive 3.0-3.5σ relations between outflow velocity and SFR, M * , and v circ . The outflow velocities scale as SFR with the range depending on whether we use a maximum or a central velocity to quantify the outflow velocity. After accounting for their increased SFR, mergers drive 32% faster outflows than nonmerging galaxies, with all of the highest velocity outflows arising from mergers. Low-mass galaxies (log (M * / M e ) < 10.5) lose some low-ionization gas through galactic outflows, while more massive galaxies retain all of their low-ionization gas, unless they undergo a merger.

show abstract

Section: Milky Way Line Fittingmentioning

confidence: 99%

Scaling Relations Between Warm Galactic Outflows and Their Host Galaxies

Chisholm¹,

Tremonti²,

Leitherer

et al. 2015

ApJ

157

211

View full text Add to dashboard Cite

show abstract

“…Supernova remnant N 132D belongs to the rare class of O-rich remnants, together with objects such as Cassiopeia A, Puppis A, or SNR 0540−69.3, and it has a kinematic age of 2500 yr (Vogt & Dopita 2011, and references therein). Its chemical composition indicates that N 132D is the remnant of the core-collapse supernova of a progenitor star with initial mass in the ∼35-75 M range (France et al 2009). The shock wave in the remnant is interacting with surrounding material, and N 132D is the brightest remnant of the LMC in X-rays (Borkowski et al 2007).…”

Section: P4: Coincident With Snr N 132dmentioning

confidence: 99%

Deep view of the Large Magellanic Cloud with six years ofFermi-LAT observations

Ackermann¹,

Albert²,

Atwood³

et al. 2016

A&A

View full text Add to dashboard Cite

Context. The nearby Large Magellanic Cloud (LMC) provides a rare opportunity of a spatially resolved view of an external star-forming galaxy in γ-rays. The LMC was detected at 0.1-100 GeV as an extended source with CGRO/EGRET and using early observations with the Fermi-LAT. The emission was found to correlate with massive star-forming regions and to be particularly bright towards 30 Doradus. Aims. Studies of the origin and transport of cosmic rays (CRs) in the Milky Way are frequently hampered by line-of-sight confusion and poor distance determination. The LMC offers a complementary way to address these questions by revealing whether and how the γ-ray emission is connected to specific objects, populations of objects, and structures in the galaxy. Methods. We revisited the γ-ray emission from the LMC using about 73 months of Fermi-LAT P7REP data in the 0.2-100 GeV range. We developed a complete spatial and spectral model of the LMC emission, for which we tested several approaches: a simple geometrical description, template-fitting, and a physically driven model for CR-induced interstellar emission. Results. In addition to identifying PSR J0540−6919 through its pulsations, we find two hard sources positionally coincident with plerion N 157B and supernova remnant N 132D, which were also detected at TeV energies with H.E.S.S. We detect an additional soft source that is currently unidentified. Extended emission dominates the total flux from the LMC. It consists of an extended component of about the size of the galaxy and additional emission from three to four regions with degree-scale sizes. If it is interpreted as CRs interacting with interstellar gas, the large-scale emission implies a large-scale population of ∼1-100 GeV CRs with a density of ∼30% of the local Galactic value. On top of that, the three to four small-scale emission regions would correspond to enhancements of the CR density by factors 2 to 6 or higher, possibly more energetic and younger populations of CRs compared to the large-scale population. An alternative explanation is that this is emission from an unresolved population of at least two dozen objects, such as pulsars and their nebulae or supernova remnants. This small-scale extended emission has a spatial distribution that does not clearly correlate with known components of the LMC, except for a possible relation to cavities and supergiant shells. Conclusions. The Fermi-LAT GeV observations allowed us to detect individual sources in the LMC. Three of the newly discovered sources are associated with rare and extreme objects. The 30 Doradus region is prominent in GeV γ-rays because PSR J0540−6919 and N 157B are strong emitters. The extended emission from the galaxy has an unexpected spatial distribution, and observations at higher energies and in radio may help to clarify its origin.

show abstract

“…The expected line width is comparable to the instrumental profile of COS for an extended source with the G160M grating, but no instrumental profile was available for extended sources other than the statement by France et al (2009) that the spectral resolution is about 200 km s −1 . The profile is not expected to be strictly Gaussian, but to be affected by the shape of the entrance aperture.…”

Section: Observations and Data Reductionmentioning

confidence: 84%

Carbon, Helium, and Proton Kinetic Temperatures in a Cygnus Loop Shock Wave

Raymond

Edgar

Ghavamian

et al. 2015

ApJ

View full text Add to dashboard Cite

Observations of SN1006 have shown that ions and electrons in the plasma behind fast supernova remnant shock waves are far from equilibrium, with the electron temperature much lower than the proton temperature and ion temperatures approximately proportional to ion mass. In the ∼360 km s −1 shock waves of the Cygnus Loop, on the other hand, electron and ion temperatures are roughly equal, and there is evidence that the oxygen kinetic temperature is not far from the proton temperature. In this paper we report observations of the He II λ1640 line and the C IV λ1550 doublet in a 360 km s −1 shock in the Cygnus Loop. While the best fit kinetic temperatures are somewhat higher than the proton temperature, the temperatures of He and C are consistent with the proton temperature and the upper limits are 0.5 and 0.3 times the mass-proportional temperatures, implying efficient thermal equilibration in this collisionless shock. The equilibration of helium and hydrogen affects the conversion between proton temperatures determined from Hα line profiles and shock speeds, and that the efficient equilibration found here reduces the shock speed estimates and the distance estimate to the Cygnus Loop of Medina et al. (2014) to about 800 pc.

show abstract

Cosmic Origins Spectrograph Observations of the Chemical Composition of SNR LMC N132d

Cited by 32 publications

References 23 publications

Scaling Relations Between Warm Galactic Outflows and Their Host Galaxies

Scaling Relations Between Warm Galactic Outflows and Their Host Galaxies

Deep view of the Large Magellanic Cloud with six years ofFermi-LAT observations

Carbon, Helium, and Proton Kinetic Temperatures in a Cygnus Loop Shock Wave

Contact Info

Product

Resources

About