High-resolution H<i>α</i> imaging of the northern Galactic plane and the IGAPS image database

Greimel, R.; Drew, J. E.; Monguió, M.; Ashley, R. P.; Barentsen, Geert; Eislöffel, J.; Mampaso, A.; Morris, Rhys; Naylor, T.; Roe, C.; Sabin, L.; Stecklum, B.; Wright, N. J.; Groot, P.; Irwin, M. J.; Barlow, M. J.; Fariña, C.; Fernández-Martín, A.; Parker, Quentin A.; Phillipps, S.; Scaringi, Simone; Zijlstra, A. A.

doi:10.1051/0004-6361/202140950

Cited by 12 publications

(5 citation statements)

References 46 publications

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“…The existing Hα surveys in the local universe have a surface brightness limit insufficient to detect the faint signals to be expected (Table 2): equal or fainter than 10 erg s cm arcsec 17 1 2 2 ----. This level is not within reach of the existing surveys (e.g., Moss et al 1988;James et al 2004;Dale et al 2008;Epinat et al 2008;Jaiswal & Omar 2016;Greimel et al 2021). Moreover, some of them are focused on the emission of the MW, either diffuse (e.g., Gaustad et al 2001) or its point-like sources (e.g., Barentsen et al 2014).…”

Section: Appendix a Expected Hα Signalsmentioning

confidence: 92%

Discovery of Faint Double-peak Hα Emission in the Halo of Low Redshift Galaxies

Alméida

Calhau

Muñoz–Tuñón

et al. 2022

ApJ

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Aimed at the detection of cosmological gas being accreted onto galaxies in the local universe, we examined the Hα emission in the halo of 164 galaxies in the field of view of the Multi-Unit Spectroscopic Explorer Wide survey (MUSE-Wide) with observable Hα (redshift <0.42). An exhaustive screening of the corresponding Hα images led us to select 118 reliable Hα emitting gas clouds. The signals are faint, with a surface brightness of 10 − 17.3 ± 0.3 erg s − 1 cm − 2 arcsec − 2 . Through statistical tests and other arguments, we ruled out that they are created by instrumental artifacts, telluric line residuals, or high-redshift interlopers. Around 38% of the time, the Hα line profile shows a double peak with the drop in intensity at the rest frame of the central galaxy, and with a typical peak-to-peak separation of the order of ±200 km s−1. Most line emission clumps are spatially unresolved. The mass of emitting gas is estimated to be between 1 and 10−3 times the stellar mass of the central galaxy. The signals are not isotropically distributed; their azimuth tends to be aligned with the major axis of the corresponding galaxy. The distances to the central galaxies are not random either. The counts drop at a distance >50 galaxy radii, which roughly corresponds to the virial radius of the central galaxy. We explore several physical scenarios to explain this Hα emission, among which accretion disks around rogue intermediate-mass black holes fit the observations best.

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Section: Appendix a Expected Hα Signalsmentioning

confidence: 92%

Discovery of Faint Double-peak Hα Emission in the Halo of Low Redshift Galaxies

Alméida

Calhau

Muñoz–Tuñón

et al. 2022

ApJ

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“…The survey produced various general photometric and imaging catalogs (González-Solares et al, 2008;Barentsen et al, 2014;Sale et al, 2014;Scaringi et al, 2018;Monguió et al, 2020;Fratta et al, 2021;Greimel et al, 2021), but it also focused on dedicated astronomical objects such as PNe for instance.…”

Section: Int Photometric Hα Surveymentioning

confidence: 99%

Exploitation of the IPHAS to Investigate Planetary Nebulae

Sabin

Toalá²,

Ramos-Larios

et al. 2022

Front. Astron. Space Sci.

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Similar to other classes of astronomical objects, there is a large discrepancy between the total count of theoretically predicted planetary nebulae (PNe) and the number of those actually observed. This discrepancy introduces bias in our attempt to globally understand and characterize the PNe population. Major efforts have been made to find the missing PNe. In particular, the INT Photometric Hα Survey (IPHAS) has, since its debut, provided a whelm of new (candidate) PNe, some of which have been studied in depth using various methodologies such as deep imaging and low- and high-resolution spectroscopy. Here, we present the outcome of the analysis of a first group of these well-investigated IPHAS PNe with a focus on the extended ones. We show that, in general, the missing objects that were expected to be unveiled by the survey (low density, evolved, and distant) are indeed discovered, but the survey also allows the retrieval of “simply” overlooked PNe.

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“…We have used the data of the INT Galactic Plane Survey (IGAPS) in order to construct a mosaic image of the 1.4×1.4 deg 2 region surrounding G121.1-1.9 in the narrow-band centred on H𝛼 emission line (Greimel et al 2021). The resulting image, built after iterative background matching and co-adding of the individual images, performed using MONTAGE software 3 , is shown in Figure A1 in Appendix.…”

Section: H𝛼mentioning

confidence: 99%

SRG/eROSITA discovery of a radio faint X-ray candidate supernova remnant SRGe J003602.3+605421=G121.1-1.9

Khabibullin¹,

Churazov²,

Bykov³

et al. 2022

Preprint

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We report the discovery of a candidate X-ray supernova remnant SRGe J003602.3+605421=G121.1-1.9 in the course of SRG/eROSITA all-sky survey. The object is located at (l,b)=(121.1 • ,-1.9 • ), is ≈ 36 arcmin in angular size and features nearly circular shape. Clear variations in spectral shape of the X-ray emission across the object are detected, with the emission from the inner (within 9') and outer (9'-18') parts dominated by iron and oxygen/neon lines, respectively. The non-equilibrium plasma emission model is capable of describing the spectrum of the outer part with the initial gas temperature 0.1 keV, final temperature 0.5 keV and the ionization age ∼ 2 × 10 10 cm −3 s. The observed spectrum of the inner region is more complicated (plausibly due to the contribution of the outer shell) and requires substantial overabundance of iron for all models we have tried. The derived X-ray absorption equals to (4 − 6) × 10 21 cm −2 , locating the object at the distance beyond 1.5 kpc, and implying its the age ∼ (5 − 30) × 1000 yrs. No bright radio, infrared, H 𝛼 or gamma-ray counterpart of this object have been found in the publicly-available archival data. A model invoking a canonical 10 51 erg SN Ia explosion in the hot and tenuous medium in outer region of the Galaxy ∼9 kpc away might explain the bulk of the observed features.This object might be a rare example of an old SN Ia remnant in our Galaxy still bearing signatures of the ejecta enrichment and probing the thermal and non-thermal properties of the hot phase of the ISM above the cold disc. This scenario can be tested with future deep X-ray and radio observations.

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High-resolution Hα imaging of the northern Galactic plane and the IGAPS image database

Cited by 12 publications

References 46 publications

Discovery of Faint Double-peak Hα Emission in the Halo of Low Redshift Galaxies

Discovery of Faint Double-peak Hα Emission in the Halo of Low Redshift Galaxies

Exploitation of the IPHAS to Investigate Planetary Nebulae

SRG/eROSITA discovery of a radio faint X-ray candidate supernova remnant SRGe J003602.3+605421=G121.1-1.9

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