Infrared properties of planetary nebulae with [WR] and wels central stars

Abstract

We report the IR properties of planetary nebulae with WR type and wels central stars known to date and compare them with the IR properties of a sample of PNe with H-rich central stars. We use near-, mid-and far-IR photometric data from archives to derive the IR properties of PNe. We have constructed IR colour-colour diagrams of PNe using measurements from 2M ASS, IRAS, W ISE and Akari bands.[WR] PNe have a larger near-IR emission from the hot dust component and also show a tendency for stronger 12µm emission as compared to the other two groups. Cool AGB dust properties of all PNe are found to be similar. We derived the dust colour temperatures, dust masses, dust-to-gas mass ratios, IR luminosities and IR excess of PNe for these three groups.[WR] PNe and wels-PNe tend to have larger mean values for dust mass when compared to the third group. The average dust-togas mass ratio is found to be similar for the three groups of PNe. While there is a strong correlation of dust temperature and IR luminosity with the age for the three groups of PNe, the dust mass, dust-to-gas mass ratios and IR excess are found to be non-varying as the PNe evolve. [WR] PNe and wels-PNe show very similar distribution of excitation classes and also show similar distribution with Galactic latitude. of emission lines from ions with different ionization potential is related to the temperature evolution and can give the evolutionary connection between [WR] stars of different subtypes. Such quantitative classification schemes of [WR] stars currently in use were given by Crowther, De Marco & Barlow (1998, CDB98) and by Acker & Neiner (2003, AN03). CDB98 find a continuity in the [WR] classification scheme from [WC] to [WO] and suggest that the sequence is primarily due to excitation rather than abundance. All subtypes are seen in a sequence of decreasing stellar temperature from [WO1] → [WO4] → [WC4] → [WC11]. AN03 conclude from this an evolution of stars from post-AGB → [WC11] → [WC4] -[WO4] → [WO1]. Both CDB98 and AN03 find a sparsity of CSPNe in the [WC6-8] subclasses indicating a rapid evolution through this range or a different evolutionary path leading to two ionization sequences which is not yet understood. On the other hand, wels do not have such a classification scheme.Though there are pronounced differences between the [WR] stars and the hydrogen rich CSPNe in their spectra and photospheric abundances etc., the PNe with [WR] stars have many properties which are very similar to those shown by the PNe with hydrogen-

A Survey for C II Emission-Line Stars in the Large Magellanic Cloud

“…There is also no imaging evidence of a planetary nebula around J0608 (M20), but one is likely present in both cases, due to the appearance of prominent forbidden lines of multiple species, and also the known association of Galactic [WC11] stars with PNe. However, while J0608 exhibits JHK colors compatible with the compendium of PNe with late-[WC] central stars given by Muthumariappan & Parthasarathy (2020) and the selection criteria of Akras et al (2019), 153-1 does not. The WISE mid-infrared colors of both of these stars do lie roughly in the ranges for this spectral type listed by Muthumariappan & Parthasarathy (2020), although the general scatter of WISE colors for these objects is quite large.…”

“…However, while J0608 exhibits JHK colors compatible with the compendium of PNe with late-[WC] central stars given by Muthumariappan & Parthasarathy (2020) and the selection criteria of Akras et al (2019), 153-1 does not. The WISE mid-infrared colors of both of these stars do lie roughly in the ranges for this spectral type listed by Muthumariappan & Parthasarathy (2020), although the general scatter of WISE colors for these objects is quite large. The catalog of van Aarle et al (2011) flags this star as a post-AGB candidate, based on Spitzer photometry.…”

Physical and Kinematical Characteristics of Wolf–Rayet Central Stars and their Host Planetary Nebulae

“…This result is consistent with the higher ionized mass, effective temperature and luminosity of the early [WR] group compared to the late [WR] group. Further, we compared the mean EC of [WRE] PNe with the non-[WR], WEL and [WR] CSs given by Muthumariappan & Parthasarathy (2020), where the result shows a slightly higher value than non-[WR] (EC = 6.6), and greater than WEL (EC = 5.2) and [WR] (EC = 4.3) nebulae.…”

“…Recently, Muthumariappan & Parthasarathy (2020) used IR photometric data to derive the IR properties of three samples of PNe associated with [WR], WEL and normal CSs. The results revealed a tight correlation of decreasing dust temperature (T d ) with nebular age: have T eff between 20,000 and 80,000 K (Danehkar 2021; and references therein).…”

Carbon dust in the evolved born-again planetary nebulae A30 and A78

“…This model predicts a dust mass of 3.6 × 10 −5 M for the inner shell and about 60 times more for the outer shell, 2.2 × 10 −3 M . Recently, Muthumariappan & Parthasarathy (2020) presented a statistical analysis of the IR properties of the PNe with Wolf-Rayettype CSPN compiled by Weidmann & Gamen (2011) using photometric measurements from the Two Micron All Sky Survey (2MASS), Wide-field Infrared Survey (WISE), Infrared Astronomical Satellite (IRAS), and Akari. This study computed the dust colour temperatures, dust masses, and dust-to-gas mass ratios, among other quantities of these PNe.…”