New DSH planetary nebulae and candidates from optical and infrared surveys

Kronberger, M.; Parker, Quentin A.; Jacoby, George H.; Acker, A.; Alves, Filipe; Bojičić, Ivan S.; Eigenthaler, Paul; Frew, David J.; Harmer, Dianne; Patchick, D.; Reid, Warren A.; Schedler, Johannes

doi:10.1088/1742-6596/728/7/072012

Cited by 22 publications

(19 citation statements)

References 5 publications

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“…Because of the lack of WISE measurements, a search for a far-IR excess was not possible for the four other stars. In the (W2−W3), (W3−W4) diagram, the WISE colors of J1556 agree with the bulk of PNe (Kronberger et al 2014). However, as mentioned above, no nebular emission lines are visible in the SDSS spectrum (total exposure time ≈2.25 h).…”

Section: Search For Nebular Lines and Infrared Excesssupporting

confidence: 67%

Radial velocity variable, hot post-AGB stars from the MUCHFUSS project

Reindl¹,

Geier

Kupfer

et al. 2016

A&A

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In the course of the MUCHFUSS project we recently discovered four radial velocity (RV) variable, hot (T eff ≈ 80 000−110 000 K) post-asymptotic giant branch (AGB) stars. Among them, we found the first known RV variable O(He) star, the only second known RV variable PG 1159 close binary candidate, as well as the first two naked (i.e., without planetary nebula (PN)) H-rich post-AGB stars of spectral type O(H) that show significant RV variations. We present a non-LTE spectral analysis of these stars along with one further O(H)-type star whose RV variations were found to be not significant. We also report the discovery of a far-infrared excess in the case of the PG 1159 star. None of the stars in our sample displays nebular emission lines, which can be explained well in terms of a very late thermal pulse evolution in the case of the PG 1159 star. The "missing" PNe around the O(H)-type stars seems strange, since we find that several central stars of PNe have much longer post-AGB times. Besides the non-ejection of a PN, the occurrence of a late thermal pulse, or the re-accretion of the PN in the previous post-AGB evolution offer possible explanations for those stars not harbouring a PN (anymore). In the case of the O(He) star J0757, we speculate that it might have been previously part of a compact He transferring binary system. In this scenario, the mass transfer must have stopped after a certain time, leaving behind a low-mass close companion that may be responsible for the extreme RV shift of 107.0 ± 22.0 km s −1 that was measured within only 31 min.

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Section: Search For Nebular Lines and Infrared Excesssupporting

confidence: 67%

Radial velocity variable, hot post-AGB stars from the MUCHFUSS project

Reindl¹,

Geier

Kupfer

et al. 2016

A&A

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“…The latter source is indicated in the SIMBAD data base 1 as a planetary nebula. For both nebulae we found optical counterparts in the Isaac Newton Telescope (INT) Photometric Hα Survey of the Northern Galactic Plane (IPHAS; Drew et al 2005), which are indicated as circumstellar matter in the Hong Kong/AAO/Strasbourg Hα (HASH) planetary nebula database (Parker, Bojičić & Frew 2016; see also Kronberger et al 2016), and named there as PNG 117.4−01.5 (or Pa 58) and PNG 035.1+02.0, respectively. WS29 is also discernable in the Digitized Sky Survey II (DSS-II; McLean et al 2000) red band image and is a known source of radio emission (Condon, Kaplan & Terzian 1999 Figure 1.…”

Section: Two Wise Nebulae and Their Central Starsmentioning

confidence: 99%

Two Circumstellar Nebulae Discovered with the Wide-field Infrared Survey Explore and Their Massive Central Stars

Gvaramadze

Kniazev

Castro

et al. 2019

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We report the discovery of two mid-infrared nebulae in the northern hemisphere with the Wide-field Infrared Survey Explorer and the results of optical spectroscopy of their central stars, BD+60 • 2668 (composed of two components, separated from each other by ≈3 arcsec) and ALS 19653, with the Calar Alto 3.5-m telescope and the Southern African Large Telescope (SALT), respectively. We classify the components of BD+60 • 2668 as stars of spectral types B0.5 II and B1.5 III. ALS 19653 is indicated in the SIMBAD data base as a planetary nebula, while our observations show that it is a massive B0.5 Ib star, possibly in a binary system. Using the stellar atmosphere code fastwind, we derived fundamental parameters of the three stars as well as their surface element abundances, implying that all of them are either on the main sequence or only recently left it. This provides further evidence that massive stars can produce circumstellar nebulae while they are still relatively unevolved. We also report the detection of optical counterparts to the mid-infrared nebulae and a second, more extended optical nebula around ALS 19653, and present the results of SALT spectroscopy of both nebulae associated with this star. The possible origin of the nebulae is discussed.

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“…• Broadband photographic imagery e.g. Abell (1966), and the recent work by the Deep-Sky Hunters (DSH) team, an amateur-professional consortium (Jacoby et al 2010;Kronberger et al 2016, and references therein). Candidates were typically identified from direct inspection of images, or the online scanned data in the case of the DSH discoveries.…”

Section: Detection Techniques Past and Presentmentioning

confidence: 99%

“…Since the last IAUS review in 2011 (Parker et al 2012), over 750 PNe and PN candidates have been found, many still needing assessment in the HASH database. Sabin et al (2014) announced the discovery of 159 true, likely and possible PNe, 284 PN candidates have been found from UWISH2 (Froebrich et al 2015; Gledhill, these proceedings), and another 180 from the DSH team and related efforts (Kronberger et al 2016;and personal communication;Acker et al 2015). Fragkou et al (2016) have found 70 candidates using radio and IR surveys, and other contributions in the infrared have been made by Flagey et al (2014), Nowak et al (2014), and Ingallinera et al (2014aIngallinera et al ( ,b, 2016 who are systematically investigating the 300+ unidentified MIPSGAL nebulae found by Mizuno et al (2010), though most remain un-assessed at the time of writing.…”

Section: Detection Techniques Past and Presentmentioning

confidence: 99%

Challenges faced by current Galactic planetary nebula surveys

Frew

2016

Proc. IAU

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Determining the demographics of the Galactic planetary nebula (PN) population is an important goal to further our understanding of this intriguing phase of stellar evolution. The Galactic population has more than doubled in number over the last 15 years, particularly from narrowband \ha\ surveys along the plane. In this review I will summarise these results, with emphasis on the time interval since the last IAU Symposium. These primarily optical surveys are not without their limitations and new surveys for PNe in the infrared similarly face a number of challenges. I will discuss the need for multi-wavelength approaches to discovery and analysis. The desire to have accurate volume-limited samples of Galactic PNe at our disposal is emphasised, which will be impacted with new data from the Gaia satellite mission. We need robust surveys of PNe and their central stars, especially volume-limited surveys, in order to clarify and quantify their evolutionary pathways.Comment: 8 pages, 3 figures, Invited Review given at IAU Symposium 323, held in Beijing, China, October 201

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New DSH planetary nebulae and candidates from optical and infrared surveys

Cited by 22 publications

References 5 publications

Radial velocity variable, hot post-AGB stars from the MUCHFUSS project

Radial velocity variable, hot post-AGB stars from the MUCHFUSS project

Two Circumstellar Nebulae Discovered with the Wide-field Infrared Survey Explore and Their Massive Central Stars

Challenges faced by current Galactic planetary nebula surveys

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