The Pan-STARRS1 Database and Data Products

Flewelling, H.; Magnier, E. A.; Chambers, K.; Heasley, J. N.; Holmberg, Conrad; Huber, M. E.; Sweeney, William E.; Waters, C.; Calamida, A.; Casertano, Stefano; Chen, X.; Farrow, Daniel J.; Hasinger, G.; Henderson, Rachel E.; Long, Knox S.; Metcalfe, N.; Narayan, Gautham; Nieto-Santisteban, María; Norberg, Peder; Rest, A.; Saglia, R.; Szalay, A. S.; Thakar, Aniruddha R.; Tonry, J.; Valenti, Jeff A.; Werner, Suzanne; White, R. L.; Denneau, L.; Draper, P. W.; Hodapp, Klaus W.; Jedicke, Robert; Kaiser, Nick; Kudritzki, Rolf‐Peter; Price, P. A.; Wainscoat, R. J.; Chastel, S.; McLean, B.; Postman, Marc; Shiao, B.

doi:10.3847/1538-4365/abb82d

Cited by 439 publications

(239 citation statements)

References 17 publications

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“…The initial source position required some refinement owing to the 8″ pixel size of PGIR. There are no counterparts in optical (e.g., PanSTARRS; Flewelling et al 2020) or near-infrared (Two Micron All Sky Survey (2MASS); Skrutskie et al 2006) survey catalogs, though a hard stretch of the 2MASS images does reveal a faint detection at K s and perhaps H. A nearby WISE catalog source at 00:52:20.41, +56:34:03.3 was determined to be the source that had brightened. The brightening is also recorded in NEOWISE (Mainzer et al 2014) data.…”

Section: Gattini 12 μM (J-band) Light Curvementioning

confidence: 98%

Outbursting Young Stellar Object PGIR 20dci in the Perseus Arm

Hillenbrand

Hankins

et al. 2021

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We report the discovery of a likely outbursting Class I young stellar object, associated with the star-forming region NGC 281-W (distance ∼2.8 kpc). The source is currently seen only at infrared wavelengths, appearing in both the Palomar Gattini InfraRed (1.2 μm) and the Near-Earth Object Wide-field Infrared Survey Explorer (3.4 and 4.6 μm) photometric time-domain surveys. Recent near-infrared imaging reveals a new, extended scattered light nebula. Recent near-infrared spectroscopy confirms the similarity of PGIR 20dci to FU Ori-type sources, based on strong molecular absorption in CO, H 2 O, and OH; weak absorption in several atomic lines; and a warm wind/ outflow as indicated by a P Cygni profile in the He I λ10830 line. This is a rare case of an FU Ori star with a wellmeasured long-term photometric rise before a sharper outburst, and the second instance of an FU Ori star with a documented two-step brightening in the mid-infrared.

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Section: Gattini 12 μM (J-band) Light Curvementioning

confidence: 98%

Outbursting Young Stellar Object PGIR 20dci in the Perseus Arm

Hillenbrand

Hankins

et al. 2021

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“…No host-galaxy subtraction was performed, which would cause no significant differences, as SN 2019muj is appeared at the edge of the galaxy. We calibrated our photometry in the Swope natural system (Krisciunas et al 2017) using photometry of stars in the same field as 2019muj from the Pan-STARRS DR1 catalogue (Flewelling et al 2016) and transformed using the Supercal method (Scolnic et al 2015). Final photometry was obtained using DoPhot (Schechter, Mateo & Saha 1993) on the reduced images.…”

Section: Photometrymentioning

confidence: 99%

SN 2019muj – a well-observed Type Iax supernova that bridges the luminosity gap of the class

Barna

Szalai

Camacho-Neves

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present early-time (t < +50 days) observations of SN 2019muj (= ASASSN-19tr), one of the best-observed members of the peculiar SN Iax class. Ultraviolet and optical photometric and optical and near-infrared spectroscopic follow-up started from ∼5 days before maximum light (tmax(B) on 58 707.8 MJD) and covers the photospheric phase. The early observations allow us to estimate the physical properties of the ejecta and characterize the possible divergence from a uniform chemical abundance structure. The estimated bolometric light curve peaks at 1.05 × 1042 erg s−1 and indicates that only 0.031 M⊙ of 56Ni was produced, making SN 2019muj a moderate luminosity object in the Iax class with peak absolute magnitude of $M_\rm {V} = -16.4$ mag. The estimated date of explosion is t0 = 58 698.2 MJD and implies a short rise time of trise = 9.6 days in B-band. We fit of the spectroscopic data by synthetic spectra, calculated via the radiative transfer code TARDIS. Adopting the partially stratified abundance template based on brighter SNe Iax provides a good match with SN 2019muj. However, without earlier spectra, the need for stratification cannot be stated in most of the elements, except carbon, which is allowed to appear in the outer layers only. SN 2019muj provides a unique opportunity to link extremely low-luminosity SNe Iax to well-studied, brighter SNe Iax.

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“…SN 2017gas appears to be close to the centre of 2MASX J20171114+5812094, so we must distinguish this object from an AGN. The host offset of SN 2017gas is 1.97 (according to PS1; Flewelling et al 2020), the host has a semimajor axis of 8.80 , and Skrutskie et al (2006) report an uncertainity of 0.23 in the centre of the host right ascension and declination. Discovery images show the transient being off-centre 3 .…”

Section: The Silver Samplementioning

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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The Pan-STARRS1 Database and Data Products

Cited by 439 publications

References 17 publications

Outbursting Young Stellar Object PGIR 20dci in the Perseus Arm

Outbursting Young Stellar Object PGIR 20dci in the Perseus Arm

SN 2019muj – a well-observed Type Iax supernova that bridges the luminosity gap of the class

A systematic reclassification of Type IIn supernovae

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