Contents

• New DQ white dwarfs in the Sloan Digital Sky Survey DR4: confirmation of two sequences
• 1 Introduction
• 2 Selection of DQ candidates
• 3 Atmospheric analysis of the DQ white dwarfs
• 4 Results and discussion
• References
• 5 Online Material
• Appendix A: Graphical display of spectral fits for 60 DQs

A&A 454, 951-956 (2006)
DOI: 10.1051/0004-6361:20065287

New DQ white dwarfs in the Sloan Digital Sky Survey DR4: confirmation of two sequences

D. Koester - S. Knist

Institut für Theoretische Physik und Astrophysik, University of Kiel, 24098 Kiel, Germany

Received 27 March 2006 / Accepted 26 April 2006

Abstract
Context. DQ white dwarfs show atomic or molecular carbon features in their spectra. The atmosphere consists of helium and the carbon is believed to be dredged-up to the surface by the deepening helium convection zone.
Aims. We want to identify new DQ in the Data Release 4 of the Sloan Digital Sky Survey, determine the effective temperatures and carbon abundances and search for systematic trends between these parameters as indication of the origin of this class.
Methods. Photometric selection criteria are developed and applied to the catalog to identify candidates, which are in a final step confirmed by visual inspection of spectra. The parameters are determined through comparison with theoretical spectra and colors.
Results. Our final DQ catalog contains 65 stars. 40 of these are new identifications, the other 25 have been described as DQ before in the literature. We derive effective temperatures and carbon abundances for 60 of these stars. The majority of stars defines a clear sequence in the C abundance vs. $T\sb {\rm eff}$ diagram, with high abundances found at high $T\sb {\rm eff}$ and vice versa. We also confirm with high significance a second sequence with an abundance about 1 dex higher at the same $T\sb {\rm eff}$, and discuss the nature and possible origin of the high-C sequence.

Key words: stars: white dwarfs - stars: abundances

1 Introduction

White dwarfs of spectral type DQ are defined as showing atomic or molecular features of carbon in a helium atmosphere. Contrary to other metals (notably Ca) found in cool white dwarfs, which are thought to be provided through an accretion process from outside the star, the most widely accepted explanation for the DQs is dredge-up from the underlying carbon/oxygen core through the expanding He convection zone (Pelletier et al. 1986; Koester et al. 1982). A detailed summary of the basic properties of this class and earlier references to spectroscopic analyses has been given recently in a comprehensive paper by Dufour et al. (2005, =DB05 henceforth) and need not be repeated here.

In addition to the general understanding of the nature, evolutionary relations and origin of the peculiar spectral types of white dwarfs, the DQs are of special interest, because they provide information about the deeper layers of the stars. The transition between the outer helium layer and the carbon/oxygen core - the result of the helium burning in the progenitor - is not abrupt, but rather gradual as determined by the diffusion equilibrium (Koester et al. 1982). We can predict the structure of this transition quantitatively (Pelletier et al. 1986), as well as the depth of the helium convection zone at a given effective temperature and mass of the star. The observed carbon abundance in the atmosphere is then directly related to the thickness of the helium layer remaining from the previous nuclear evolution, which is a very important parameter for the understanding of stellar evolution. The first estimate of this thickness by Pelletier et al. (1986) - $\log M_{\rm He}/M \approx -3.75$ - was much thinner than predicted by evolutionary calculations of the AGB phase. However, the recent abundance determinations by DB05, together with the new models of the outer layers by Fontaine & Brassard (2005) are in much better agreement with theoretical expectations. Nevertheless, there are still many problems understanding the detailed connection of the DQ stars to possible helium-rich progenitors (Althaus et al. 2005; Scóccola et al. 2006).

When searching for correlations of DQ parameters, e.g. between atmospheric carbon abundance and effective temperature, it is very helpful to have available a homogeneous sample of observations. It has been found in previous studies that abundances determined from atomic lines in the UV or molecular bands in the optical may sometimes differ significantly (e.g. Provencal et al. 2002), possibly blurring any correlation if only one or the other observation is available for different objects (Weidemann & Koester 1995). Such a homogeneous sample is currently provided by the Sloan Digital Sky Survey, and DB05 provides the first quantitative analysis of 40 DQs from the Data Release 1 (DR1). In this paper we report similar results for 40 new DQs (and 20 previously known) extracted from DR4 (Adelman-McCarthy et al. 2006).

2 Selection of DQ candidates

DR4 of the SDSS contains spectra for approximately 240 000 objects classified as "point source'' or "unknown''. In order to narrow down this huge database to tractable numbers we have applied three consecutive selection steps, the first two based on the SDSS photometry, the last on the spectra.

2.1 DQ regions in SDSS color space and theoretical models

Theoretical SDSS colors can be calculated from synthetic spectra by convolving them with the 5 ugriz SDSS band passes. Our model grid is similar to that described in Carollo et al. (2003), but extended to cover effective temperatures from 13 000 K to 4400 K. Logarithmic C abundance by number relative to He (=[C/He]) range from -8 to -4in steps of 0.5. The standard grid used here has a surface gravity of $\log g$ = 8.00, but additional grids were calculated with 7.5 and 8.5 for comparison. The models are fully blanketed, fully including the line and molecular band absorption in the calculation of the atmospheric structure. Non-ideal effects in the form of a lowering of the dissociation energy of the C₂ molecule is included in a very approximate way.

The transmission curves for the five filters (for airmass 1.3 as recommended) were obtained from the SDSS web sites; the zero-points for the magnitudes were set to correspond to the AB system of magnitudes (Fukugita et al. 1996) except for small changes to u,i,z(-0.04, 0.01, 0.02) similar to those discussed in Eisenstein et al. (2006).

The dependence on $T\sb {\rm eff}$ and [C/He] is strongest in the u-gvs. g-r two-color diagram and much less in the remaining independent indices used, r-i and i-z. Figure 1 shows this diagram with the theoretical grid, and 40 observed DQs from Harris et al. (2003) and Kleinman et al. (2004), which indeed fall in or very near the theoretical grid. Note that we have not applied any correction for galactic extinction (see DB05).

Figure 1: Theoretical SDSS color grid for DQ white dwarfs. Thick continuous lines are lines of constant carbon abundance from [C/He] = -8.0 ( top) to -4 ( bottom), step 1.0. Thin dashed: lines of constant $T\sb {\rm eff}$ from 4400 K ( right) to 13 000 K ( left) in steps of 200 K. Crosses show the observed DQ stars from Harris et al. (2003) and Kleinman et al. (2004).

 

 

Table 1: 40 new DQ white dwarfs. The first columns give the SDSS name and internal designation. Next is effective temperature determined from a fit to the photometry. The carbon abundance [C/He] is determined from a model fit to the spectrum, keeping the temperature fixed. The final column gives a classification and remarks. WD 1105+412 and WD 0913+103 are reclassified from a DC classification in McCook & Sion (1999). GD 311 is classified DC in Kawka & Vennes (2006), but we believe very weak Swan bands to be present. SDSS J133127.04+670419.5 is classified DC in Kleinman et al. (2004).

SDSS name	MJD	Plate	Fid	$\hbox{$T\sb{\rm eff}$ }$ [K]	[C/He]	$\sigma$ [C/He]	Spectral type/Ref
SDSS J074204.79+434835.7	53 052	1736	139	7738	-5.47	0.04	DQ
SDSS J084131.55+332915.6	52 642	933	16	6810	-6.62	0.05	DQ
SDSS J085239.66+042804.5	52 670	1190	177	9555			DQ
SDSS J085506.62+063904.7	52 668	1189	535	7337	-5.99	0.01	DQ
SDSS J085709.01+060357.4	52 668	1189	27	8210	-5.00	0.02	DQ
SDSS J090449.73+395416.4	52 703	1199	595	7319	-5.74	0.05	DQ
SDSS J090514.78+090426.5	52 973	1300	420	8861	-4.89	0.01	DQ (H$\alpha$?)
SDSS J090632.17+470235.8	52 606	898	565	5070	-4.31	0.01	DQ (weak bands)
SDSS J091602.73+101110.5	53 050	1739	592	8715	-4.81	0.01	DQ
SDSS J091830.27+484323.0	52 637	900	429	8884	-3.72	0.06	DQ
SDSS J092153.46+342136.9	52 995	1274	216	8202	-5.46	0.09	DQ
SDSS J092613.46+472521.1	52 637	900	41	7261	-6.41	0.06	DQ
SDSS J092909.03+331011.7	52 991	1593	94	6361	-5.57	0.01	DQ
SDSS J094014.65+090641.8	52 993	1304	45	6169	-7.34	0.05	DQpec (rounded bands)
SDSS J094115.18+090154.4	52 993	1304	9	9122	-4.73	0.02	DQ
SDSS J094138.08+441458.2	52 672	1202	58	8113	-5.42	0.06	DQ
SDSS J095934.95+453725.4	52 703	942	446	7211	-5.52	0.06	DQ
SDSS J100059.82+100531.7	53 053	1308	307	7958	-4.83	0.02	DQ, WD 1105+412
SDSS J101750.38+373637.5	52 996	1427	216	7497	-5.79	0.03	DQ
SDSS J101800.00+083820.3	52 762	1237	621	7784	-5.85	0.01	DQ
SDSS J102635.81+580714.8	52 316	559	6	8879	-4.56	0.03	DQ
SDSS J110759.46+405910.9	53 046	1437	512	7169	-6.45	0.02	DQ
SDSS J110912.21+424956.0	53 053	1363	37	9402	-4.84	0.08	DQ, WD 0913+103
SDSS J112604.29+441938.6	53 062	1365	564	7097	-6.38	0.05	DQ
SDSS J113534.61+572451.7	53 033	1310	485	7385	-6.42	0.02	GD 311, Kawka & Vennes (2006)
SDSS J115149.92+452729.8	53 084	1368	503	8829	-4.75	0.04	DQ
SDSS J122545.87+470613.0	53 117	1451	35	6109	-5.82	0.01	DQ
SDSS J123347.60+125346.1	53 169	1616	429	7152	-6.36	0.02	DQ
SDSS J130945.62+444541.0	53 084	1375	391	8085	-4.01	0.03	DQ
SDSS J131534.72+471108.9	53 062	1461	428	7524	-5.99	0.01	DQ
SDSS J131930.66+140137.1	53 112	1773	105	7626	-5.65	0.05	DQ
SDSS J133127.04+670419.5	51 988	496	583	8899	-4.91	0.06	DQ (weak bands), Kleinman et al. (2004)
SDSS J143144.83+375011.9	53 089	1381	599	6173	-6.97	0.02	DQ
SDSS J152812.05+513445.2	52 378	795	319	7531	-5.69	0.03	DQ
SDSS J153447.54+414559.4	53 149	1679	616	7804	-5.92	0.02	DQZ (CaII)
SDSS J161653.36+392444.4	52 759	1336	572	7319	-5.92	0.02	DQ
SDSS J165436.86+315754.4	52 791	1176	238	7258	-5.89	0.01	DQ
SDSS J171341.76+324009.1	52 413	976	623	7901	-5.36	0.01	DQ
SDSS J211130.04-003628.8	52 431	985	35	7168	-6.27	0.05	DQ
SDSS J213503.32+000318.4	52 468	989	198	6413	-6.78	0.03	DQ

 

 

Table 2: 25 rediscovered DQ white dwarfs in the same format as Table 1. 20 of these are analyzed also in DB05. Information on the remaining 5 can be found in the McCook & Sion (1999) catalog (WD 1426+613), Liebert et al. (2003), Carollo et al. (2006), and Harris et al. (2003).

SDSS name	MJD	Plate	Fid	$\hbox{$T\sb{\rm eff}$ }$ [K]	[C/He]	$\sigma$ [C/He]	Spectral type/Ref
SDSS J000011.57-085008.4	52 143	650	450	8042	-5.46	0.08
SDSS J000807.54-103405.6	52 141	651	199	7768	-5.66	0.06
SDSS J002531.50-110800.9	52 145	653	86	8367	-4.96	0.01
SDSS J015433.57-004047.2	51 871	403	268	7435	-5.89	0.03
SDSS J015441.75+140308.0	51 877	430	558	6511	-6.89	0.01
SDSS J032054.11-071625.4	51 924	460	236	6266	-5.45
SDSS J033218.22-003722.1	51 810	415	240	8600	-4.62	0.03
SDSS J090157.92+575135.9	51 924	483	600				Liebert et al. (2003)
SDSS J091922.18+023605.0	51 929	473	458	11566
SDSS J093537.00+002422.0	52 314	476	461	4958	-6.19	0.02	Harris et al. (2003)
SDSS J094004.64+021022.6	52 026	477	493	7283	-5.95	0.01
SDSS J095137.60+624348.7	51 943	487	227	8388	-5.11	0.10
SDSS J113359.94+633113.2	52 059	597	139	12082
SDSS J114851.68-012612.8	52 056	329	578	9174	-3.73	0.01
SDSS J125359.61+013925.6	52 026	523	252	8282	-4.98	0.02
SDSS J123752.12+415625.8	53 090	1454	146	5846	-5.51	0.01	Carollo et al. (2006)
SDSS J132858.20+590851.0	52 411	959	504				Liebert et al. (2003)
SDSS J142728.30+611026.4	52 368	607	379	6427	-6.83	0.01	WD 1426+613
SDSS J144407.25+043446.8	52 026	587	418	9449	-3.65	0.05
SDSS J144808.07-004755.9	51 662	308	145	7063	-6.50	0.04
SDSS J154810.66+562647.7	52 072	617	551	8119	-5.46	0.07
SDSS J155413.53+033634.5	52 023	595	373	6512	-6.94	0.03
SDSS J164328.54+400204.3	52 050	630	386	7144	-6.20	0.07
SDSS J165538.51+372247.1	52 071	632	92	8997	-4.75	0.06
SDSS J205316.34-070204.3	52 176	636	267	6382	-5.45	0.02

Using this information about the position of DQs in the SDSS color space, we have, as a first selection step, extracted from the SDSS database all objects in the "point source'' and "unknown'' categories falling into the region defined by

$$-0.8 < u-g < 1.5 \mbox{\qquad and \qquad} -0.8 < g-r < 1.5,$$

resulting in 86 856 selected objects. This sample still contains large numbers of DA white dwarfs and quasars. We therefore have, in a second step, refined the color region using a polygon in the u-g, g-rplane. The polygon area follows rather closely the outline of the theoretical grid, except at the hot end. Since the grid converges towards a single line (the models are much less dependent on the C abundance) the polygon at the hot end is significantly wider in u-g. Applying this selection step narrowed the candidate sample down to 44 928 objects.

2.2 Selection in 4-dimensional color space

Since we consider for the moment only the dependence of colors on $T\sb {\rm eff}$ and [C/He], it is obvious that the theoretical grid must define a 2-dimensional surface in the 4-dimensional color space ( u-g,g-r,r-i,i-z). That the variation is strongest in the first two components suggests that this surface might be approximated by a plane and this is confirmed by looking at different projections of the grid in two- or three-dimensional subspaces. We have therefore fitted a plane to the nodes of this grid using a $\chi^2$ minimization technique. The fit is extremely good, with typical deviations of grid points from the plane of 0.03 mag.

The equation of the plane is

$$\left(\begin{array}{c} u-g \\ g-r\\ r-i\\ i-z\end{array}\righ... ...} 1.00000\\ -0.00006\\ -0.02747\\ 0.14871 \end{array} \right)$$

where we have used the first two colors directly as the two variables for the plane. The reasonable region for DQs is given by the limits

$$-0.55 < u-g < 1.3 \mbox{\qquad and \qquad} -0.3 < g-r < 1.4.$$

This plane representation of theoretical DQ colors was used in the final photometric selection step. We defined a minimum "distance'' d from the plane for each observed object by measuring each coordinate in units of their individual measurement errors

$$d^2 = \sum_{i=1}^{4}\left(\frac{c_{\rm ob}(i)-c_{\rm th}(i)}{\sigma(i)}\right)^2 \cdot$$

Here $c_{\rm ob}$ and $c_{\rm th}$ are the four observed and theoretical SDSS colors, and $\sigma$ the measurement error of the observation. We eliminated the majority of objects by using a limit of d=6.5. This limit had been determined from a test using the 40 DQs of Fig. 1. The final sample contained 6952 DQ candidates.

2.3 Color space for different surface gravities

We have also fitted the theoretical grids for $\log g$ = 7.5 and 8.5 in the same way. The resulting planes were practically indistinguishable from the $\log g$ = 8.0 plane, however, the lines of constant temperature or C abundance are slightly shifted. This corresponds to the well known fact for DQs that the parameters $\log g$ and [C/H] are degenerate. They cannot both be determined from photometry (nor spectra), because a change of $\log g$ can always be very nearly compensated with a corresponding change of [C/He], and one of the two has to be assumed to be able to proceed. Using the fact that most white dwarfs cluster around 0.6  $M\sb{\odot}$, we have assumed $\log g$ = 8, as did DB05.

2.4 Visual classification of the 6952 candidates

Spectra for all remaining candidates were extracted from the SDSS database and inspected visually. More than 95% turned out to be quasars, easily recognized by their strong and broad emission lines. Of the remaining objects some were DA white dwarfs (broad Balmer absorption), some galaxies with narrow absorption lines. The DQs, the topic of this study, were identified through their molecular Swan bands. In total we found 65 DQs, of which 25 were already known in the literature, 36 are new detections, and 4 reclassifications from a spectral type of DC.

Tables 1 and 2 list all 65 DQ with their SDSS names, internal identifiers, and atmospheric parameters, determined as described in the next section. Most of the objects show only carbon features. SDSS J090514.78+090426.5 shows a feature near the position of H$\alpha$, but nothing near the other Balmer lines, and the presence of hydrogen is highly uncertain. SDSS J153447.54+414559.4 shows Ca II H and K lines with equivalent widths of 2.1 and 1.0 Å. The wings are broad and the distance of the star is very likely less than 100 pc, implying a photospheric origin of the lines, probably due to accretion. SDSS J094014.65+090641.8 shows rounded bands similar to SDSS J223224.0-074434.3 in Harris et al. (2003).

3 Atmospheric analysis of the DQ white dwarfs

3.1 Photometry

The parameters $T\sb {\rm eff}$ and [C/He] were determined by minimizing in the sense of a $\chi^2$ the distance between the observed point in 4-dimensional color space with model colors interpolated on the $T\sb {\rm eff}$ - [C/He] grid. $\chi^2$ minimization was obtained with the AMOEBA routine from Press et al. (1992). Since our sample contains 20 objects in common with DB05, we compare the derived $T\sb {\rm eff}$ in Fig. 2. The agreement in $T\sb {\rm eff}$ with those from DB05, which are based on photometry and spectra is excellent, confirming that photometry alone already gives a reliable $T\sb {\rm eff}$. From the differences between the two completely independent determinations we estimate a typical error for $T\sb {\rm eff}$ of 190 K. This is a much more realistic error than the internal errors from the $\chi^2$ routine; it is also very similar to the $T\sb {\rm eff}$ error of 170 K cited by DB05, and we take this as our error estimate for $T\sb {\rm eff}$. On the other hand, the derived carbon abundances differ markedly, with a much higher scatter and also systematic differences. This is not really surprising, since the colors for different abundances converge at the high temperature end and a [C/He] determination based on colors alone will be inaccurate to impossible. In addition, small uncertainties of the magnitude zero-points could shift the whole grid by a few hundreds of a magnitude, resulting in systematic changes. These abundances are not used further and therefore not shown here.

Figure 2: Comparison of effective temperatures determined from the photometry with results from DB05.

3.2 Spectroscopy

Fortunately, SDSS provides photometry and spectroscopy. The spectra were fitted with the theoretical spectra from our standard grid using the same methods used by us for other types of white dwarfs (Homeier et al. 1998; Koester et al. 2001). In principle the spectroscopic fit provides $T\sb {\rm eff}$ and [C/He] ($\log g$ = 8 is always assumed). However, since the flux calibration of the spectra is not completely reliable and the molecular features depend strongly on both, temperature and carbon abundance, the photometric observations provide a much more stringent constraint for the temperature. Our current codes cannot simultaneously fit spectra and photometric data. We have therefore chosen to keep the temperature fixed at the photometric solution (shown above to be reliable) and to determine only the carbon abundance from the spectra. Since the photometric temperature determination errors are smaller than those obtained by fitting both temperature and abundance from the spectra, this results also in smaller errors of the final C abundances. These abundances are given in Tables 1 and 2. For the five objects with missing entries in the [C/He] column we could not obtain reasonable fits within our grid. Two examples for the spectral fits for the region around the strongest Swan bands are shown in Fig. 3. All fits of the 60 objects are shown in the electronic online version of the paper; the abundances are also given in Tables 1 and 2.

Figure 3: Two examples of the spectral fitting for objects with molecular features of different strengths. Top: SDSS J171341.76+324009.1, bottom: SDSS J032054.11-071625.4. Note that the name used above the panels is the internal SDSS-MJD-PLATE-FID designation of the SDSS project, which can be cross-identified using Tables 1 and 2. Vertical axis is relative intensity on an arbitrary scale.

Figure 4: Comparison of carbon abundances from spectral fitting with results from DB05.

Figure 4 gives a comparison of our final results for the carbon abundance with DB05 for the common objects. The general agreement is very good, with a small systematic shift of about 0.2 dex, increasing from lower to high abundances. The [C/He] abundances of DB05 are on average slightly higher than our values.

4 Results and discussion

We have identified 40 new DQ white dwarfs and rediscovered another 25 from the Data Release 4 of the Sloan Digital Sky Survey and presented effective temperatures and carbon abundances for 60 of them. This increases very significantly the number of DQs with a careful analysis using up-to-date model atmospheres. Particularly important is the fact that our sample is based on a completely homogeneous set of photometry and spectra. This is similar to the work of DB05, who however included also observations from other sources together with 40 SDSS objects in their sample. For the objects in common with their analysis we find good agreement for the parameters, with a slight offset in the abundances of the order of 0.2 dex.

Figure 5: Carbon abundance versus effective temperatures. Full circles are the results from this paper. We have added as open circles the results from DB05 for those objects not in our sample.

The major result of this paper is shown in Fig. 5, which displays the carbon abundance versus effective temperature. In addition to our own results (shown as full circles) we have here included data from DB05 for those objects not included in our sample (open circles). We clearly confirm the three main conclusions of DB05:

• The paucity of objects with $T\sb {\rm eff}$ below 6000 K. Our sample adds only one object clearly below the apparent cutoff, also carbon-rich as the single cool objects in DB05.
• The clear sequence for the majority of the objects, from low  $T\sb {\rm eff}$, low [C/He] to high $T\sb {\rm eff}$, high [C/He], indicated by the lower of the two regression line fits (these fits use only the results from this paper). The existence of this sequence was first pointed out by DB05 and shows the large advantage of using a homogeneous sample of good quality observations compared to e.g. the study of Weidemann & Koester (1995). The extrapolation of the sequence to 10 000 K predicts [C/He] = -4.0, in agreement with the theoretical calculations of Fontaine & Brassard (2005) for a He-layer thickness of 10^-4 of the stellar mass.
• The existence of a separate population of carbon-rich DQs, with an abundance about 1 dex higher than the primary sequence. This population seems to form a second sequence, which we have tentatively described with the upper regression line.

Based on one single object with a parallax and thus mass determination of 1.05  $M\sb{\odot}$ in the upper sequence (G47-18 = WD 0856+33), DB05 tentatively suggested that all objects of this group are massive white dwarfs and might be the descendants of the hot DQ stars, which also seem to be massive, although that assertion is also only based on two objects (Macdonald et al. 1998; Liebert et al. 2003; Weidemann 2005). Stellar evolution calculations predict smaller He envelope masses for more massive progenitors (Kawai et al. 1988) and might lead to the dredge-up occurring at higher effective temperatures (Thejll et al. 1990). This would also be a natural explanation for the absence of the high-mass tail in the DB mass distribution (Beauchamp et al. 1996; Liebert et al. 2003).

While these conclusions seem rather speculative at present, it is obvious that further study of the large number of DQs with excellent observations coming from SDSS and other large scale surveys will provide important clues for the remaining open question of the origin and evolution of white dwarf surface compositions and spectral types. Of particular importance are parallax determinations for DQs on the high abundance sequence.

Acknowledgements

This study was partially supported by a grant from the Deutsche Forschungsgemeinschaft (KO731/21-1,-2), and would have been impossible without the SDSS. Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Korean Scientist Group, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France

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5 Online Material

Appendix A: Graphical display of spectral fits for 60 DQs

Thin blue line: observed spectra, thick red: model. Vertical axis is relative intensity on an arbitrary scale. The spectra are not in the same sequence as in Tables 1 and 2, since the intensity scales differ and similar spectra are grouped together. However, the objects can be cross-identified using the internal SDSS-MJD-PLATE-FID designation on top of each panel.

Figure A.1: Spectral fit for DQ white dwarfs.

Figure A.1: continued.

Figure A.1: continued.

Figure A.1: continued.

Figure A.1: continued.

Figure A.1: continued.

Figure A.1: continued.

Figure A.1: continued.

Figure A.1: continued.