scholarly journals Supersoft X-ray nebulae in the Large Magellanic Cloud

2020 ◽  
Vol 497 (3) ◽  
pp. 3234-3250 ◽  
Author(s):  
Diego A Farias ◽  
Alejandro Clocchiatti ◽  
Tyrone E Woods ◽  
Armin Rest
Keyword(s):  
Interstellar Medium ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
The Other ◽  
X Rays ◽  
X Ray ◽  
Upper Limits ◽  
Type Ia ◽  
Source Models ◽  
Flux Measurements

ABSTRACT Supersoft X-rays sources (SSSs) have been proposed as potential Type Ia supernova (SN Ia) progenitors. If such objects are indeed persistently X-ray luminous and embedded in sufficiently dense interstellar medium (ISM), they will be surrounded by extended nebular emission. These nebulae should persist even long after an SN Ia explosion, due to the long recombination and cooling times involved. With this in mind, we searched for nebular [O iii] emission around four SSSs and three SNRs in the Large Magellanic Cloud, using the 6.5-m Baade telescope at Las Campanas Observatory and the imacs camera. We confirm that, out of the four SSS candidates, only CAL 83 can be associated with an [O iii] nebula. The [O iii] luminosity for the other objects is constrained to ≲17 per cent of that of CAL 83 at 6.8 pc from the central source. Models computed with the photoionization code cloudy indicate that either the ISM densities in the environments of CAL 87, RX J0550.0-7151, and RX J0513.9-6951 must be significantly lower than surrounding CAL 83 or the average X-ray luminosities of these sources over the last ≲10  000 yr must be significantly lower than presently observed, in order to be consistent with the observed luminosity upper limits. For the three SNRs we consider (all with ages <1000 yr), our [O iii] flux measurements together with the known surrounding ISM densities strongly constrain the ionizing luminosity of their progenitors in the last several thousand years, independent of the progenitor channel.

X-rays from superbubbles in the Large Magellanic Cloud

1991 ◽  
Vol 148 ◽  
pp. 99-100
Author(s):  
You-Hua Chu ◽  
Mordecai-Mark Mac Low
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Shell Structures ◽  
X Rays ◽  
Simple Ring ◽  
X Ray ◽  
Order Of Magnitude

We find diffuse X-ray emission not associated with known SNRs in seven LMC HII complexes. All, except 30 Dor, have simple ring morphologies, indicating shell structures. Assuming these are superbubbles, we find the X-ray luminosity expected from their hot interiors to be an order of magnitude lower than the observed value. SNRs close to the center of a superbubble add very little emission, but we calculate that off-center SNRs hitting the ionized shell could explain the observed emission.

scholarly journals Excluding supersoft X-ray sources as progenitors for four Type Ia supernovae in the Large Magellanic Cloud

2019 ◽  
Vol 484 (1) ◽  
pp. 1317-1324 ◽  
Author(s):  
J Kuuttila ◽  
M Gilfanov ◽  
I R Seitenzahl ◽  
T E Woods ◽  
F P A Vogt
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Type Ia Supernovae ◽  
X Ray ◽  
Type Ia ◽  
Ia Supernovae

scholarly journals IRAS Observations of Collisionally Heated Dust in Large Magellanic Cloud Supernova Remnants

1988 ◽  
Vol 101 ◽  
pp. 383-386
Author(s):  
James R. Graham ◽  
A. Evans ◽  
J.S. Albinson ◽  
M.F. Bode ◽  
W.P.S. Meikle
Keyword(s):  
Interstellar Medium ◽  
Supernova Remnants ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Substantial Fraction ◽  
X Ray ◽  
Ir Sources ◽  
Atomic Cooling ◽  
Dust Grain ◽  
Ir Emission

AbstractIRAS additional observations show that luminous (104−105 L⊙) far-IR sources are associated with the Large Magellanic Cloud (LMC) supernova remnants N63A, N49, N49B, and N186D. Comparison of the IRAS and X-ray data shows that a substantial fraction of the IR emission from three of the SNRs can be accounted for by collisionally heated dust. The ratio of dust-grain cooling to total atomic cooling is ~10 in X-ray emitting gas (T~106 K). We show why dust cooling does not dominate, but probably speeds SNR evolution in an inhomogeneous interstellar medium.

The detection of X-rays from the hot interstellar medium of the Large Magellanic Cloud

1991 ◽  
Vol 374 ◽  
pp. 475 ◽  
Author(s):  
Q. Wang ◽  
T. Hamilton ◽  
D. J. Helfand ◽  
X. Wu
Keyword(s):  
Interstellar Medium ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
X Rays

X-Rays from Superbubbles in the Large Magellanic Cloud. III. X-Ray--dim Superbubbles

1995 ◽  
Vol 450 ◽  
pp. 157 ◽  
Author(s):  
You-Hua Chu ◽  
Hsiao-Wei Chang ◽  
Yu-Ling Su ◽  
Mordecai-Mark Mac Low
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
X Rays ◽  
X Ray

scholarly journals Multi-wavelength View of the Interstellar Medium in the Large Magellanic Cloud

1998 ◽  
Vol 15 (1) ◽  
pp. 136-140
Author(s):  
You-Hua Chu
Keyword(s):  
Interstellar Medium ◽  
Supernova Remnants ◽  
Optical Emission ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Radio Continuum ◽  
Emission Lines ◽  
X Rays ◽  
Multi Wavelength ◽  
The Relationship

AbstractThe Large Magellanic Cloud (LMC) has been surveyed in optical emission lines, X-rays, radio continuum, HI, and CO lines. These surveys provide views of the interstellar medium (ISM) in the LMC of unprecedented clarity, allowing us to study astrophysical processes and to examine the relationship among the different phases of the ISM. Multi-wavelength images are used to illustrate the physical structures of supernova remnants, superbubbles, and supergiant shells, as well as the global interstellar structure of the LMC.

scholarly journals Discovery of an ∼30-yr-duration post-nova pulsating supersoft source in the Large Magellanic Cloud

2020 ◽  
Vol 499 (2) ◽  
pp. 2007-2014
Author(s):  
G Vasilopoulos ◽  
F Koliopanos ◽  
T E Woods ◽  
F Haberl ◽  
M D Soraisam ◽  
...  
Keyword(s):  
White Dwarf ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
X Ray ◽  
Short Period ◽  
Type Ia ◽  
Nuclear Burning ◽  
Soft Spectrum ◽  
Binary Evolution ◽  
First Time

ABSTRACT Supersoft X-ray sources (SSS) have been identified as white dwarfs accreting from binary companions and undergoing nuclear burning of the accreted material on their surface. Although expected to be a relatively numerous population from both binary evolution models and their identification as type Ia supernova progenitor candidates, given the very soft spectrum of SSSs relatively few are known. Here we report on the X-ray and optical properties of 1RXS J050526.3−684628, a previously unidentified accreting nuclear-burning white dwarf located in the Large Magellanic Cloud (LMC). XMM–Newton observations enabled us to study its X-ray spectrum and measure for the first time short-period oscillations of ∼170 s. By analysing newly obtained X-ray data by eROSITA, together with Swift observations and archival ROSAT data, we have followed its long-term evolution over the last 3 decades. We identify 1RXS J050526.3−684628 as a slowly evolving post-nova SSS undergoing residual surface nuclear burning, which finally reached its peak in 2013 and is now declining. Though long expected on theoretical grounds, such long-lived residual-burning objects had not yet been found. By comparison with existing models, we find that the effective temperature and luminosity evolution are consistent with an ∼0.7 M⊙ carbon–oxygen white dwarf accreting ${\sim} 10^{-9}~\rm {M}_{\odot }$ yr−1. Our results suggest that there may be many more undiscovered SSSs and ‘missed’ novae awaiting dedicated deep X-ray searches in the LMC and elsewhere.

scholarly journals An X-ray image of the Large Magellanic Cloud: detection of the hot interstellar medium

1991 ◽  
Vol 148 ◽  
pp. 37-44
Author(s):  
D. J. Helfand
Keyword(s):  
Energy Balance ◽  
Interstellar Medium ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Imaging Data ◽  
Cloud Detection ◽  
X Ray ◽  
X Ray Imaging ◽  
30 Doradus

We report the results of a comprehensive reanalysis of the X-ray imaging data for the Large Magellanic Cloud obtained with the Einstein Observatory. A map covering 37 deg2 of the Cloud is presented. The total 0.15–3.5 keV luminosity is ˜ 5 × 1038erg s--1, two thirds of which can be attributed to the 105 identified discrete emitters and the remainder of which arise from the coronal component of the interstellar medium at temperatures from ˜ 2 to ˜ 10 × 106K. The energy balance for this hot ISM and the morphology of specific regions such as 30 Doradus and LMC-2 are briefly discussed.

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