Two new nova shells associated with V4362 Sagittarii and DO Aquilae

Harvey, E. J.; Redman, M. P.; Boumis, P.; Akras, S.; Fitzgerald, Karol; Dulaimi, Salam E. Hammeed; Williams, S. C.; Darnley, M. J.; Lam, Marco C.; Kopsacheilli, M.; Derlopa, S.

doi:10.1093/mnras/staa2896

Cited by 15 publications

(11 citation statements)

References 102 publications

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“…On the other hand, this distance is closer (although still larger) to the one derived from Gaia EDR3 of 0.90 +0.35 −0.20 kpc (Bailer-Jones et al 2021), being both distances consistent at 1𝜎. Note that the determination of Gaia distances for stars surrounded by unresolved diffuse emission has been questioned (e.g., Kimeswenger & Barría 2018;Harvey et al 2020), as red targets with nebular remnant or high-brightness nebulosities show a much larger parallax dispersion, systematically underestimating the errors of objects with circumstellar material in the Gaia DR2 database.…”

Section: Distancesupporting

confidence: 47%

QU Vul: An Integral Field Spectroscopy Case Study of a Nova Shell

Santamaría¹,

Guerrero²,

A.³

et al. 2022

Preprint

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We present GTC MEGARA high-dispersion integral field spectroscopic observations of the nova remnant QU Vul, which provide a comprehensive 3D view of this nova shell. The tomographic analysis of the H𝛼 emission reveals a complex physical structure characterized by an inhomogeneous and clumpy distribution of the material within this shell. The overall structure can be described as a prolate ellipsoid with an axial ratio of 1.4±0.2, a major axis inclination with the line of sight of 12 • ± 6 • , and polar and equatorial expansion velocities ≈560 km s −1 and 400±60 km s −1 , respectively. The comparison of the expansion velocity on the plane of the sky with the angular expansion implies a distance of 1.43±0.23 kpc. The ionized mass is found to be ≈ 2 × 10 −4 M , noting that the information on the 3D distribution of material within the nova shell has allowed us to reduce the uncertainty on its filling factor. The nova shell is still in its free expansion phase, which can be expected as the ejecta mass is much larger than the swept-up circumstellar medium mass. The 3D distribution and radial velocity of material within the nova shell provide an interpretation of the so-called "castellated" line profiles observed in early optical spectra of nova shells, which can be attributed to knots and clumps moving radially along different directions.

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Section: Distancesupporting

confidence: 47%

QU Vul: An Integral Field Spectroscopy Case Study of a Nova Shell

Santamaría¹,

Guerrero²,

A.³

et al. 2022

Preprint

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show abstract

“…Indeed, there seems to be a variety of H profile shapes observed which may result from the CSM having a variety of different geometries, with the inclination to the line of sight also having an effect. Harvey et al (2020) shows how different shell morphologies can affect line profiles. An example of a deviation from a symmetrical profile is shown in the middle spectral epochs of SN 2009ip (Fig.…”

Section: Discussion and Summarymentioning

confidence: 99%

A systematic reclassification of Type IIn supernovae

Ransome

Habergham-Mawson

Darnley

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Type IIn supernovae (SNe IIn) are a relatively infrequently observed subclass of SNe whose photometric and spectroscopic properties are varied. A common thread among SNe IIn are the complex multiple-component hydrogen Balmer lines. Owing to the heterogeneity of SNe IIn, online databases contain some outdated, erroneous, or even contradictory classifications. SN IIn classification is further complicated by SN “impostors” and contamination from underlying H ii regions. We have compiled a catalogue of systematically classified nearby (redshift z < 0.02) SNe IIn using the Open Supernova Catalogue (OSC). We present spectral classifications for 115 objects previously classified as SNe IIn. Our classification is based upon results obtained by fitting multiple Gaussians to the Hα profiles. We compare classifications reported by the OSC and Transient Name Server (TNS) along with the best matched templates from SNID. We find that 28 objects have been misclassified as SNe IIn. TNS and OSC can be unreliable; they disagree on the classifications of 51 of the objects and contain a number of erroneous classifications. Furthermore, OSC and TNS hold misclassifications for 34 and twelve (respectively) of the transients we classify as SNe IIn. In total, we classify 87 SNe IIn. We highlight the importance of ensuring that online databases remain up to date when new or even contemporaneous data become available. Our work shows the great range of spectral properties and features that SNe IIn exhibit, which may be linked to multiple progenitor channels and environment diversity. We set out a classification sche me for SNe IIn based on the Hα profile which is not greatly affected by the inhomogeneity of SNe IIn.

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“…Indeed, there seems to be a variety of H𝛼 profile shapes observed which may result from the CSM having a variety of different geometries, with the inclination to the line of sight also having an effect. Harvey et al (2020) shows how different shell morphologies can affect line profiles. An example of a deviation from a symmetrical profile is shown in the middle spectral epochs of SN 2009ip (Fig.…”

Section: Discussion and Summarymentioning

confidence: 99%

A systematic reclassification of type IIn supernovae

Ransome,

Habergham-Mawson,

Darnley

et al. 2021

Preprint

View full text Add to dashboard Cite

Type IIn supernovae (SNe IIn) are a relatively infrequently observed subclass of SNe whose photometric and spectroscopic properties are varied. A common thread among SNe IIn are the complex multiple-component hydrogen Balmer lines. Owing to the heterogeneity of SNe IIn, online databases contain some outdated, erroneous, or even contradictory classifications. SN IIn classification is further complicated by SN "impostors" and contamination from underlying H regions. We have compiled a catalogue of systematically classified nearby (redshift 𝑧 < 0.02) SNe IIn using the Open Supernova Catalogue (OSC). We present spectral classifications for 115 objects previously classified as SNe IIn. Our classification is based upon results obtained by fitting multiple Gaussians to the H𝛼 profiles. We compare classifications reported by the OSC and Transient Name Server (TNS) along with the best matched templates from SNID. We find that 28 objects have been misclassified as SNe IIn. TNS and OSC can be unreliable; they disagree on the classifications of 51 of the objects and contain a number of erroneous classifications. Furthermore, OSC and TNS hold misclassifications for 34 and twelve (respectively) of the transients we classify as SNe IIn. In total, we classify 87 SNe IIn. We highlight the importance of ensuring that online databases remain up to date when new or even contemporaneous data become available. Our work shows the great range of spectral properties and features that SNe IIn exhibit, which may be linked to multiple progenitor channels and environment diversity. We set out a classification sche me for SNe IIn based on the H𝛼 profile which is not greatly affected by the inhomogeneity of SNe IIn.

show abstract

Two new nova shells associated with V4362 Sagittarii and DO Aquilae

Cited by 15 publications

References 102 publications

QU Vul: An Integral Field Spectroscopy Case Study of a Nova Shell

QU Vul: An Integral Field Spectroscopy Case Study of a Nova Shell

A systematic reclassification of Type IIn supernovae

A systematic reclassification of type IIn supernovae

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