A Search for Diffuse Bands in the Circumstellar Envelopes of Post-AGB Stars ,
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A&A 480, 133–148 (2008) Astronomy DOI: 10.1051/0004-6361:20065282 & c ESO 2008 Astrophysics A search for diffuse bands in the circumstellar envelopes of post-AGB stars, R. Luna1,N.L.J.Cox2,M.A.Satorre1, D. A. García Hernández3,O.Suárez4, and P. García Lario2 1 Laboratorio de Astrofísica Experimental, Escuela Politécnica Superior de Alcoy, Universidad Politécnica de Valencia, Plaza de Ferrándiz y Carbonell, 03801 Alcoy, Alicante, Spain e-mail: [email protected] 2 Herschel Science Centre, Research and Scientific Support Department of ESA, European Space Astronomy Centre, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain 3 W. J. McDonald Observatory. The University of Texas at Austin. 1 University Station, C1400. Austin, TX 78712-0259, USA 4 LUAN, Université de Nice Sophia Antipolis, Parc Valrose, 06108 Nice Cedex 2, France Received 27 March 2006 / Accepted 6 November 2007 ABSTRACT In this work we present the results of a systematic search for diffuse bands (DBs, hereafter) in the circumstellar envelopes of a carefully selected sample of post-AGB stars. We concentrated on analyzing 9 of the DBs most commonly found in the interstellar medium. The strength of these features is determined using high-resolution optical spectroscopy, and the results obtained are compared with literature data on field stars affected only by interstellar reddening. Based on the weak features observed in the subsample of post- AGB stars dominated by circumstellar reddening, we conclude that the carrier(s) of these DBs must not be present in the circumstellar environment of these sources, or at least not under the excitation conditions in which DBs are formed. This conclusion is applicable to all the post-AGB stars studied, irrespective of the dominant chemistry or the spectral type of the star considered. A detailed radial velocity analysis of the features observed in individual sources confirms this result, as the Doppler shifts measured are found to be consistent with an interstellar origin. Key words. stars: AGB and post-AGB – ISM: dust, extinction 1. Introduction (Foing & Ehrenfreund 1994; Iglesias-Groth 2007), and / or buck- yonions (Iglesias-Groth 2004), are promising candidates. The lo- The diffuse interstellar bands (DIBs) are absorption features, cal interstellar environmental conditions set the balance of local showing a broad range of widths and strengths, which appear formation and destruction of the carriers, as well as their level over-imposed on the spectra of bright stars whose lines of of ionisation and hydrogenation. The interstellar radiation field sight probe (extra)galactic diffuse-to-dense interstellar clouds. is one of the most important factors in this (Ruiterkamp et al. Currently, more than 200 DIBs have been identified and cata- 2005). logued in the spectral range from 3600 to 10 200 Å (Jenniskens There is a possible link between the DIB carriers and the & Désert 1994; Cox et al. 2005), the most studied ones being carriers of the unidentified (aromatic) infrared bands (UIBs), the those found at 4430, 5780, 5797, and 6284 Å. Since their dis- so-called PAH-DIB hypothesis (Crawford et al. 1985; Leger & covery (Heger 1922), they have been associated to the interstel- D’Hendecourt 1985; Van der Zwet & Allamandola 1985). Thus, lar medium (ISM), because their strengths show a positive re- although PAHs are thought to reside and to be processed (ion- lationship with the observed extinction (Merrill 1936), as well isation, dehydrogenation, destruction) in the diffuse ISM, this as to the neutral sodium column density (Herbig 1993). Many does not exclude the scenario that these molecules (or their par- carriers have been proposed, however, no unambiguous identi- ent species) are produced elsewhere. Since circumstellar shells fication has yet been made and it is debated whether they arise are sources of replenishment of the ISM, it has been argued that from the dust or the gas components of the ISM (see reviews DIBs (and/or parent structures) may have a circumstellar origin, by Herbig 1995 and Sarre 2006). There is increasing obser- either in dense stellar winds or circumstellar shells, thus some- vational evidence that the DIB carriers constitute a set of car- how contravening the name they were initially given. The sus- bonaceous gas-phase molecules as shown from substructures re- pected connection between DIB carriers and some carbon-rich sembling rotational contours in some bands (Sarre et al. 1995; compounds can be investigated attending to the usually known Ehrenfreund & Foing 1996). In particular, photo-UV-resistant chemistry and physical properties of these circumstellar shells. organic molecules, such as carbon chains (Douglas 1977), PAHs Observationally, the detection of diffuse bands (DBs, here- (Salama et al. 1999; Allamandola et al. 1999), fullerenes after) around evolved stars is hampered by the fact that most of them are losing mass and are usually strongly variable and sur- Based on observations collected at the European Southern rounded by very cool extended atmospheres where molecules Observatory (Chile) and at the Spanish Observatorio del Roque de los are the dominant source of opacity. These stars are very dif- Muchachos of the Instituto de Astrofísica de Canarias. ficult to model, and DBs are hardly detected (in absorption) Tables 5–8 are only available in electronic form at against the forest of features attributed to molecular transitions http://www.aanda.org that appear superimposed on the stellar continuum. This has Article published by EDP Sciences 134 R. Luna et al.: A search for diffuse bands in post-AGB stars hampered any systematic search for DBs in evolved stars in the relative high galactic latitudes and are as such only affected by past. Furthermore, if detected, it is difficult to determine whether low interstellar reddening. This facilitates the attribution of a cir- the DBs are originating from the interstellar or the circumstellar cumstellar origin to the features observed. environment, or even both. The potential formation of DBs around post-AGB stars has, In the face of these difficulties, Snow & Wallerstein (1972) however, so far only been explored occasionally and for a lim- and Snow (1973) searched for circumstellar diffuse bands ited number of sources. Nevertheless, the presence of strong DBs (at 4430, 5780, 5797, and 6614 Å) in 26 stars with suspected has been reported in the optical spectra of a few post-AGB stars circumstellar dust shells / envelopes but found no evidence (Le Bertre & Lequeux 1993; García-Lario et al. 1999; Zacs et al. of their presence. Several other authors have since searched 1999a, 2001; Klochkova et al. 1999, 2000; Kendall et al. 2002) for and commented on the presence of diffuse bands and and some carbon-rich (barium) stars (Zacs et al. 2003). In several their interstellar or circumstellar nature, in spectra observed to- cases, tentative claims have been put forward for DBs detected wards planetary nebulae (NGC 6210, NGC 7027, IC 351, and at radial velocities coinciding with the photospheric absorption AFGL 2688 by Prichet & Grillmair 1984; IRAS 21282+5050 lines or shell/envelope expansion velocity (IRAS 04296+3429 by Cohen & Jones 1987; NGC 7027 and IRAS 21282+5050 by Klochkova et al. 1999; and HD 179821 by Zacs et al. 1999a). by Le Bertre & Lequeux 1992), a post-AGB star (HR 4049; All other studies listed above gave non-conclusive results. Waters et al. 1989), and a carbon star (IRAS 07270-1921 or Another method recently employed utilised nearby back- CGCS 1732; Le Bertre 1990). Le Bertre & Lequeux (1993) ground stars to probe the circumstellar environments of the studied a new sample consisting of carbon-, oxygen-, or carbon star IRC+10216 (Kendall et al. 2002) and the helix nitrogen-rich mass-losing sources, such as (pre)planetary neb- PN (Mauron & Kendall 2004). Again, no circumstellar DBs ulae (BD+30 3639, CPD-56 8032, Hen 104), a carbon-rich were detected, confirming the lack of DIB carriers in these RV Tauri star (AC Her), Wolf-Rayet stars (WR137, WR140), environments. and post-AGB stars (HR 4049, HD 213985), revisiting several In this work we present the first systematic survey to detect sources studied in the past (e.g. CS 776, NCG 7027, HR 4049, the circumstellar DBs (DCBs) in a carefully selected sample of IRAS 21282+5050). These authors did not find any evidence galactic post-AGB stars1. The goal is to perform a detailed anal- of circumstellar DBs, which refuted previous claims, and thus ysis of the differential properties observed in the DBs associ- concluded that DBs are depleted in circumstellar environments. ated to post-AGB stars in comparison with the standard DBs Notably, these authors did not detect any bands in the spectra observed towards reddened, early-type field stars (where these of sources showing strong PAH emission (UIB) at mid-infrared bands are expected to be essentially of interstellar origin). wavelengths. This suggested that carrier molecules, if present, in To perform this task we studied the intensity of 9 of circumstellar envelopes are in a different state of ionisation / hy- the strongest absorption features identified as DBs in the drogenation than in the ISM. Strong DBs were detected toward spectral range 4000−10 000 Å using high-resolution optical carbon-rich sources that do not show PAH emission, as well spectroscopy. The comparison of the properties observed in as toward most of their oxygen-rich and nitrogen-rich sources carbon-rich and oxygen-rich post-AGB stars is used to test the in the sample, although in all cases the observed DBs could carbon-rich nature of the DB carrier(s) and determine which of be attributed to the interstellar material in the lines of sight. the detected DBs are most probably of circumstellar origin (if For unexplained reasons, enhanced DBs were detected toward any). WN stars and LBVs.