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An automated method for planetary nebula detection with SIGNALS: first applications to NGC 4214 and NGC 4449;



Tekijät: Yang, Nancy; Hartke, Johanna; Bureau, Martin; Spiniello, Chiara; Guite, Louis-Simon; Flint, Guy; Arnaboldi, Magda; Ennis, Ana Ines; Martin, R. Pierre; Martin, Thomas; Robert, Carmelle; Rousseau-Nepton, Laurie; Valenzuela, Lucas M.; Vicens-Mouret, Sebastien

Kustantaja: Oxford University Press

Julkaisuvuosi: 2026

Lehti: Monthly Notices of the Royal Astronomical Society

Artikkelin numero: stag661

Vuosikerta: 548

Numero: 4

ISSN: 0035-8711

eISSN: 1365-2966

DOI: https://doi.org/10.1093/mnras/stag661

Julkaisun avoimuus kirjaamishetkellä: Avoimesti saatavilla

Julkaisukanavan avoimuus : Kokonaan avoin julkaisukanava

Verkko-osoite: https://academic.oup.com/mnras/article/548/4/stag661/8650714

Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/526482840

Rinnakkaistallenteen lisenssi: CC BY

Rinnakkaistallennetun julkaisun versio: Kustantajan versio


Tiivistelmä

Utilizing the optical imaging Fourier transform spectrograph SITELLE, the Star-formation, Ionized Gas and Nebular Abundances Legacy Survey (SIGNALS) is designed to study the connection between star-forming regions and their environments. Targeting 31 local star-forming galaxies, its data products also lend themselves to planetary nebula (PN) surveys. We present here a new pipeline to find PNe using automated emission-line diagnostics and morphology tests, that is able to distinguish PNe from contaminants with an accuracy similar to that of past visual methods. We also perform thorough completeness tests using mock PNe inserted into the data cubes with full spectra. We apply these tools to a pilot sample of two dwarf irregular galaxies from the SIGNALS survey, NGC 4214 and NGC 4449, with other galaxies to follow. For these two galaxies, we identify 25 PNe (including six new discoveries) and 23 PNe (including 13 new discoveries), respectively, and calculate PN luminosity function distances of 3.09+0.25−0.46 and 3.91+0.33−0.52 Mpc, respectively, the latter consistent with previous estimates. We also calculate the bolometric PN specific frequency of our galaxies (⁠⁠), as well as a newly defined V-band PN specific frequency (⁠⁠) based solely on the galaxies’ total luminosities in that band.



Avainsanat:
galaxies: distances and redshifts, galaxies: irregular, planetary nebulae: general

Ladattava julkaisu

This is an electronic reprint of the original article.
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Julkaisussa olevat rahoitustiedot: 
JH and CS acknowledge the financial support from the Visitor and Mobility programme of the Finnish Centre for Astronomy with ESO (FINCA). JH also acknowledges financial support from the Turku Collegium for Science, Medicine, and Technology (TCSMT) in the form of a starting grant.
The collaboration is grateful to the FRQNT, CFHT, the Canada Research Chair programme, the National Science Foundation NSF – 2109124, Natural Sciences and Engineering Research Council of Canada NSERC – RGPIN-2023-03487, the Swedish Research Council, the Swedish National Space Board, the Royal Society, and the Newton Fund via the award of a Royal Society-Newton Advanced Fellowship (NAF\R1\180403), FAPESC, CNPq, FAPESP (2014/11156-4), FAPESB (7916/2015), and CONACyT (CB2015-254132).


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