- ID:
- ivo://CDS.VizieR/J/ApJ/886/99
- Title:
- HST obs. in the region of 3 young LMC SNIa remnants
- Short Name:
- J/ApJ/886/99
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have used two methods to search for surviving companions of Type Ia supernova progenitors in three Balmer-dominated supernova remnants in the Large Magellanic Cloud: 0519-69.0, 0505-67.9 (DEM L71), and 0548-70.4. In the first method, we use the Hubble Space Telescope photometric measurements of stars to construct color-magnitude diagrams (CMDs) and compare positions of stars in the CMDs with those expected from theoretical post-impact evolution of surviving main-sequence or helium star companions. No obvious candidates of surviving companions are identified in this photometric search. Future models for surviving red giant companions or with different explosion mechanisms are needed for thorough comparisons with these observations in order to make more definitive conclusions. In the second method, we use Multi Unit Spectroscopic Explorer observations of 0519-69.0 and DEM L71 to carry out spectroscopic analyses of stars in order to use large peculiar radial velocities as diagnostics of surviving companions. We find a star in 0519-69.0 and a star in DEM L71 moving at radial velocities of 182+/-0km/s and 213+/-0km/s, respectively, more than 2.5{sigma} from the mean radial velocity of the underlying stellar population, 264 and 270km/s, respectively. These stars need higher-quality spectra to investigate their abundances and rotation velocities to determine whether they are indeed surviving companions of the supernova progenitors.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/ApJ/788/55
- Title:
- HST/WFC3 SNR discoveries in M83 (NGC5236)
- Short Name:
- J/ApJ/788/55
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present an optical/NIR imaging survey of the face-on spiral galaxy M83, using data from the Hubble Space Telescope Wide Field Camera 3 (WFC3). Seven fields are used to cover a large fraction of the inner disk, with observations in nine broadband and narrowband filters. In conjunction with a deep Chandra survey and other new radio and optical ground-based work, these data enable a broad range of science projects to be pursued. We provide an overview of the WFC3 data and processing and then delve into one topic, the population of young supernova remnants (SNRs). We used a search method targeted toward soft X-ray sources to identify 26 new SNRs. Many compact emission nebulae detected in [FeII]1.644{mu}m align with known remnants and this diagnostic has also been used to identify many new remnants, some of which are hard to find with optical images. We include 37 previously identified SNRs that the data reveal to be <0.5" in angular size and thus are difficult to characterize from ground-based data. The emission line ratios seen in most of these objects are consistent with shocks in dense interstellar material rather than showing evidence of ejecta. We suggest that the overall high elemental abundances in combination with high interstellar medium pressures in M83 are responsible for this result.
- ID:
- ivo://CDS.VizieR/J/ApJ/788/122
- Title:
- IR photometry of YSO candidates toward SNR IC 443
- Short Name:
- J/ApJ/788/122
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have carried out ^12^CO, ^13^CO, and C^18^O observations toward the mixed morphology supernova remnant (SNR) IC 443. The observations cover a 1.5{deg}x1.5{deg} area and allow us to investigate the overall molecular environment of the remnant. Some northern and northeastern partial shell structure of CO gas is around the remnant. One of the partial shells, about 5' extending beyond the northeastern border of the remnant's bright radio shell, seems to just confine the faint radio halo. On the other hand, some faint CO clumps can be discerned along the eastern boundary of the faint remnant's radio halo. Connecting the eastern CO clumps, the northeastern partial shell structures, and the northern CO partial shell, we can see that a half molecular ring structure appears to surround the remnant. The LSR velocity of the half-ring structure is in the range of -5 km/s to -2 km/s, which is consistent with that of the -4 km/s molecular clouds. We suggest that the half-ring structure of the CO emission at V_LSR_~-4 km/s is associated with the SNR. The structures are possibly swept up by the stellar winds of SNR IC 443's massive progenitor. Based on the Wide-field Infrared Survey Explorer and the Two Micron All Sky Survey near-IR database, 62 young stellar object (YSO) candidates are selected within the radio halo of the remnant. These YSO candidates concentrated along the boundary of the remnant's bright radio shell are likely to be triggered by the stellar winds from the massive progenitor of SNR IC 443.
- ID:
- ivo://CDS.VizieR/J/ApJ/866/139
- Title:
- Knots in the deep [FeII]+[SiI] image of the SNR Cas A
- Short Name:
- J/ApJ/866/139
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a long-exposure (~10hr), narrowband image of the supernova (SN) remnant Cassiopeia A (Cas A) centered at 1.644{mu}m emission. The passband contains [FeII] 1.644{mu}m and [SiI] 1.645{mu}m lines, and our "deep [FeII]+[SiI] image" provides an unprecedented panoramic view of Cas A, showing both shocked and unshocked SN ejecta, together with shocked circumstellar medium at subarcsecond (~0.7" or 0.012pc) resolution. The diffuse emission from the unshocked SN ejecta has a form of clumps, filaments, and arcs, and their spatial distribution correlates well with that of the Spitzer [SiII] infrared emission, suggesting that the emission is likely due to [SiI] not [FeII] as in shocked material. The structure of the optically invisible western area of Cas A is clearly seen for the first time. The area is filled with many quasi-stationary flocculi (QSFs) and fragments of the disrupted ejecta shell. We identified 309 knots in the deep [FeII]+[SiI] image and classified them into QSFs and fast-moving knots (FMKs). The comparison with previous optical plates indicates that the lifetime of most QSFs is >~60yr. The total H+He mass of QSFs is ~0.23M_{sun}_, implying that the mass fraction of dense clumps in the progenitor's mass ejection immediately prior to the SN explosion is about 4%-6%. FMKs in the deep [FeII]+[SiI] image mostly correspond to S-rich ejecta knots in optical studies, while those outside the southeastern disrupted ejecta shell appear Fe-rich. The mass of the [FeII] line emitting, shocked dense Fe ejecta is ~3x10^-5^M_{sun}_.
- ID:
- ivo://CDS.VizieR/J/ApJ/813/39
- Title:
- LIGO gravitational-wave (GW) searches from SNRs
- Short Name:
- J/ApJ/813/39
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We describe directed searches for continuous gravitational waves (GWs) in data from the sixth Laser Interferometer Gravitational-wave Observatory (LIGO) science data run. The targets were nine young supernova remnants not associated with pulsars; eight of the remnants are associated with non-pulsing suspected neutron stars. One target's parameters are uncertain enough to warrant two searches, for a total of 10. Each search covered a broad band of frequencies and first and second frequency derivatives for a fixed sky direction. The searches coherently integrated data from the two LIGO interferometers over time spans from 5.3-25.3 days using the matched-filtering F-statistic. We found no evidence of GW signals. We set 95% confidence upper limits as strong (low) as 4x10^-25^ on intrinsic strain, 2x10^-7^ on fiducial ellipticity, and 4x10^-5^ on r-mode amplitude. These beat the indirect limits from energy conservation and are within the range of theoretical predictions for neutron-star ellipticities and r-mode amplitudes.
- ID:
- ivo://CDS.VizieR/J/AJ/131/2525
- Title:
- MAGPIS 20cm survey
- Short Name:
- J/AJ/131/2525
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the Multi-Array Galactic Plane Imaging Survey (MAGPIS), which maps portions of the first Galactic quadrant with an angular resolution, sensitivity, and dynamic range that surpass existing radio images of the Milky Way by more than an order of magnitude. The source detection threshold at 20cm is in the range 12mJy over the 85% of the survey region (5{deg}<l<32{deg}, |b|<0.8{deg}) not covered by bright extended emission; the angular resolution is ~6". We catalog over 3000 discrete sources (diameters mostly <30") and present an atlas of ~400 diffuse emission regions. New and archival data at 90cm for the whole survey area are also presented. Comparison of our catalogs and images with the Midcourse Space Experiment mid-infrared data allows us to provide preliminary discrimination between thermal and nonthermal sources. We identify 49 high-probability supernova remnant candidates, increasing by a factor of 7 the number of known remnants with diameters smaller than 5' in the survey region; several are pulsar wind nebula candidates and/or very small diameter remnants (D<45").
- ID:
- ivo://CDS.VizieR/J/ApJ/881/54
- Title:
- Masses of SNR progenitors in M83
- Short Name:
- J/ApJ/881/54
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We determine the ages of the young, resolved stellar populations at the locations of 237 optically identified supernova remnants in M83. These age distributions put constraints on the progenitor masses of the supernovae that produced 199 of the remnants. The other 38 show no evidence for having a young progenitor and are therefore good Type Ia SNR candidates. Starting from Hubble Space Telescope broadband imaging, we measured resolved stellar photometry of seven archival WFC3/UVIS fields in F336W, F438W, and F814W. We generate color-magnitude diagrams of the stars within 50pc of each SNR and fit them with stellar evolution models to obtain the population ages. From these ages we infer the progenitor mass that corresponds to the lifetime of the most prominent age within the past 50Myr. In this sample, there are 47 SNRs with best-fit progenitor masses >15M_{sun}_, and 5 of these are >15M_{sun}_ at 84% confidence. This is the largest collection of high-mass progenitors to date, including our highest-mass progenitor inference found so far, with a constraint of <8Myr. Overall, the distribution of progenitor masses has a power-law index of -3.0_-0.7_^+0.2^, steeper than Salpeter initial mass function (-2.35). It remains unclear whether the reason for the low number of high-mass progenitors is due to the difficulty of finding and measuring such objects or because only a fraction of very massive stars produce supernovae.
- ID:
- ivo://CDS.VizieR/J/ApJ/668/906
- Title:
- Massive clumps in NGC 6334
- Short Name:
- J/ApJ/668/906
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report observations of dust continuum emission at 1.2mm toward the star-forming region NGC 6334 made with the SEST SIMBA bolometer array. The observations cover an area of ~2deg^2^ with approximately uniform noise. We detected 181 clumps spanning almost 3 orders of magnitude in mass (3-6x10^3^M_{sun}_) and with sizes in the range 0.1-1.0pc.
- ID:
- ivo://CDS.VizieR/J/MNRAS/329/775
- Title:
- 330MHz flux of 4 SNR near Galactic Centre
- Short Name:
- J/MNRAS/329/775
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have observed two fields - Field I (l=3.2{deg}, b=1.0{deg}) and Field II (l=356.8{deg}, b=-0.1{deg}) - with the Giant Metrewave Radio Telescope (GMRT) at 330MHz. In the first field, we have studied the candidate supernova remnant (SNR) G3.1-0.6 and, based on its observed morphology, spectral index and polarization, confirmed it to be an SNR. We find this supernova to have a double ring appearance with a strip of emission on its western side passing through its centre. We have discovered two extended curved objects in the second field, which appears to be part of a large shell-like structure. It is possibly the remains of an old supernova in the region. Three suspected SNRs, G356.3-0.3, G356.6+0.1 and G357.1-0.2, detected in the MOST 843-MHz survey of the GC region appear to be located on this shell-like structure. While both G356.3-0.3 and G356.6+0.1 seem to be parts of this shell, G357.1-0.2, which has a steeper spectrum above 1GHz, could be a background SNR seen through the region. Our Hi absorption observation towards the candidate SNR G357.1-0.2 indicates that it is at a distance of more than 6kpc from us.
- ID:
- ivo://CDS.VizieR/J/ApJ/855/140
- Title:
- MMT spectra of SNRs and SNR candidates in M33
- Short Name:
- J/ApJ/855/140
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- To date, over 220 emission nebulae in M33 have been identified as supernova remnants (SNRs) or SNR candidates, principally through [SII]:H{alpha} line ratios that are elevated compared to those in HII regions. In many cases, the determination of a high [SII]:H{alpha} line ratio was made using narrow-band interference filter images and has not been confirmed spectroscopically. Here, we present MMT 6.5m optical spectra that we use to measure [SII]:H{alpha} and other line ratios in an attempt to determine the nature of these suggested candidates. Of the 197 objects in our sample, 120 have no previously published spectroscopic observations. We confirm that the majority of candidate SNRs have emission line ratios characteristic of SNRs. While no candidates show Doppler-broadened lines expected from young, ejecta-dominated SNRs (>~1000km/s), a substantial number do exhibit lines that are broader than HII regions. We argue that the majority of the objects with high [SII]:H{alpha} line ratios (>0.4) are indeed SNRs, but the distinction between HII regions and SNRs becomes less obvious at low surface brightness, and additional criteria, such as X-ray detection, are needed. We discuss the properties of the sample as a whole and compare it with similar samples in other nearby galaxies.
