ALESSI 95 AND THE SHORT PERIOD CEPHEID SU CASSIOPEIAE

Alessi 95 and the Short Period Cepheid Su Cassiopeiae

Abstract

The parameters for the newly-discovered open cluster Alessi 95 are established on the basis of available photometric and spectroscopic data, in conjunction with new observations. Colour excesses for spectroscopically-observed B and A-type stars near SU Cas follow a reddening relation described by , implying a value of for the associated dust. Alessi 95 has a mean reddening of s.e., an intrinsic distance modulus of s.e. ( s.d.), pc, and an estimated age of yr from ZAMS fitting of available UBV, CCD BV, NOMAD, and 2MASS JHK observations of cluster stars. SU Cas is a likely cluster member, with an inferred space reddening of and a luminosity of s.e., consistent with overtone pulsation (), as also implied by the Cepheid’s light curve parameters, rate of period increase, and Hipparcos parallaxes for cluster stars. There is excellent agreement of the distance estimates for SU Cas inferred from cluster ZAMS fitting, its pulsation parallax derived from the infrared surface brightness technique, and Hipparcos parallaxes, which all agree to within a few percent.

Galaxy: open clusters and associations: individual: Alessi 95—stars: variables: Cepheids—stars: individual: SU Cas.

1 Introduction

When van den Bergh (1966) compiled a list of relatively bright stars visible in the National Geographic-Palomar Observatory Sky Survey (POSS) that are associated with reflection nebulosity, he noted that the distance and luminosity for one such star, the Cepheid SU Cas, might be estimated using spectroscopic and photometric observations of the nearby B-type stars HD 17138 and HD 17443, which appear to illuminate a portion of the same dust complex. His discovery was very important, given the complete lack in existing surveys of Galactic clusters lying within several degrees of the Cepheid that might serve as distance indicators. Curiously, the field of SU Cas was not surveyed in van den Bergh’s earlier search of the POSS for previously-undetected star clusters (van den Bergh, 1957).

Figure 1: A composite colour image of Alessi 95 centred on 2000.0 co-ordinates 02:52:15.1, +68:53:19, compiled by Noel Carboni from Palomar Observatory Sky Survey-2 blue, red, and near infrared images. SU Cas is the bright star near the centre of the image; the red star southwest of it is the K0 III star TE 10.

The sparse group of B stars was subsequently designated as Cas R2, and used by Racine & van den Bergh (1970) with other R-associations to map local spiral structure in the Galaxy. An initial estimate for the distance to the dust complex by Racine (1968) yielded a value of pc from spectroscopic distance moduli for the three B-type stars HD 17327, HD 17443, and HD 17706, and the bright M giant HD 23475. A later study by Schmidt (1978) using Strömgren and H photometry implied that HD 17327 and HD 17443 were closer than HD 17706, at a mean distance of pc, versus pc for the latter. Schmidt’s result found support in an independent earlier survey by Havlen (1971) of B-type stars lying within of SU Cas. Only a few were found to lie at distances comparable to that expected for SU Cas, provided it was assumed to be either a fundamental mode or overtone pulsator. A more detailed study of Cas R2 stars by Turner & Evans (1984) included an additional star, HD 16893, associated with reflection nebulosity and an A-type companion to HD 17327, yielding a small group of five stars, with five additional candidates, lying at an estimated distance of pc. It was noted that background B-type stars were plentiful in the field, with most, including HD 17706, congregating at distances of pc.

The inferred luminosity for SU Cas requires an estimate of its reddening, but the immediate field of the Cepheid was surveyed by Turner (1984, see also ()), and the field reddening appeared to be fairly well established, although with some dependence on localized dust obscuration. Several of the surveyed companions to SU Cas were found to have intrinsic distance moduli near 8.0, but there were no suspicions at the time that the Cepheid might be embedded in an anonymous open cluster. The situation changed dramatically a few years ago when Bruno Alessi discovered a sparse cluster of stars surrounding SU Cas and centred at J2000.0 co-ordinates 02:52:15.1, +68:53:19 (Alessi, 2006), as shown in Fig. 1. The cluster, designated Alessi 95, has nuclear and coronal radii of and , respectively, and was discovered from an analysis of on-line databases (see Alessi, Moitinho & Dias, 2003; Kronberger et al., 2006). The colour image (Fig. 1) emphasises the large number of blue stars (B and A-type) dominating the central regions of the cluster, and also provides a clear picture of the relationship between SU Cas and its reflection nebula with the surrounding dust.

This study was initiated in order to provide additional information about Alessi 95 — its reddening, distance, and age — based upon available observational material, and to discuss what it reveals about SU Cas. For example, the revised Hipparcos parallax of mas for SU Cas (van Leeuwen, 2007) implies a distance of pc to the Cepheid, consistent with intrinsic distance moduli near 8.0 found for several of its optical companions. It may therefore be possible to establish the distance to SU Cas via trigonometric, open cluster, and pulsation parallaxes, which would solidly anchor the short-period end of the Galactic calibration of the Cepheid period-luminosity relation and strengthen the relationship established by Turner (2010) from open clusters and associations.

2 Observational Data and Analysis

An informative set of observations for bright B-type stars in the field of SU Cas was obtained four decades ago by Havlen (1971), who made photoelectric UBV measures for 31 of 33 stars lying within of the Cepheid on two nights in September 1968 with the 0.9m telescope at Stewart Observatory. Spectroscopic observations for 25 of the stars (up to 3 spectrograms) were obtained at a dispersion of 63 Å mm with the No. 1, 0.9m telescope at Kitt Peak National Observatory (KPNO) during the summer of 1968. The spectra were measured for radial velocity and classified by Havlen (1971) using the facilities of KPNO, and also remeasured for radial velocity using the PDS microdensitometer at the University of Toronto, and reclassified by the lead author, for use in the study by Turner et al. (1985). Part of the latter study included Strömgren and H photometry for the stars obtained by Forbes using the automatic photometer on the 0.76m telescope of the Behlen Observatory at the University of Nebraska, the same facility used in the study by Schmidt (1978).

Star V B–V U–B Sp.T.
HD 11529 4.98 –0.09 –0.42 B7 IV 0.03 0.05
HD 11744 7.82 +0.38 –0.31 B3 III: 0.58 0.47
HD 12301 5.61 +0.38 –0.28 B7 Ib 0.44 0.30
HD 12509 7.09 +0.34 –0.53 B1 II 0.58 0.46
HD 12567 8.32 +0.39 –0.54 B0.5 III 0.67 0.50
HD 12882 7.58 +0.37 –0.50 B6 Iae 0.45
HD 13590 8.01 +0.38 –0.37 B2 IIIe 0.62 0.53
HD 13630 8.80 +0.36 +0.06 B8 V 0.45 0.36
HD 14010 7.14 +0.60 –0.10 B8 Iab 0.63 0.43
HD 14863 7.76 +0.06 –0.40 B5 V 0.22 0.18
HD 14980 9.10 +0.42 +0.02 A0 III: 0.42
HD 15472 7.88 +0.06 –0.61 B3 Ve 0.26
HD 15727 8.25 +0.50 –0.20 B3 III:nn 0.70 0.58
HD 16036 8.19 +0.44 +0.27 B9 Vn 0.50 0.45
HD 16393 7.59 +0.04 –0.31 B7 Vnn 0.16 0.11
HD 16440 7.89 +0.75 +0.10: B3 Vn 0.95 0.81
HD 16831 8.96 +0.32 +0.17 A5 Vp 0.16 0.07
HD 16893 8.53 +0.39 +0.37 A3 V 0.30 0.26
HD 16907 8.39: +0.13 –0.07 B9.5 V 0.16
HD 17179 7.92: +0.26: –0.39: B3 Vn 0.46
HD 17327 7.49 +0.35 –0.03 B8 III 0.44 0.40
HD 17327b 10.33 +0.51 A2 Vn 0.45
HD 17443 8.74 +0.30 +0.13 B9 V 0.36 0.31
HD 17706 8.45 +0.38 –0.18 B5 IV 0.54 0.43
HD 17856 8.71 +0.31 +0.18 B9.5 Vn 0.34 0.25
HD 17857 7.75 +0.79 +0.03 B8 Ib 0.82
HD 17929 7.84 +0.29 –0.15 B9 III 0.35 0.19
HD 17982 8.07 +0.43 +0.39 A1 V 0.40 0.34
HD 19065 5.90 –0.02 –0.13 B9 V 0.04 0.05
HD 19856 8.85 +0.21 –0.25 B6 III 0.35 0.34
HD 20226 8.62 +0.25 –0.17 B7 IV 0.37 0.30
HD 20336 4.86 –0.13 –0.75 B2 Vne 0.11 0.11
HD 20566 8.08 +0.38 –0.24 B3 Vne 0.58 0.47
HD 20710 7.61 +0.08 –0.19 B8 V 0.17 0.11
HD 21267 8.00 +0.00 –0.29 B7.5 V 0.11 0.09
HD 21725 9.12 +0.21 +0.10 B9.5 V 0.24 0.17
HD 21930 8.44 +0.19 +0.02 B9 VmA3 0.25 0.20
HD 23475 4.47 +1.88 +2.13 M2 IIa 0.27
BD+68193 9.48 +0.32 +0.02 B9.5 IV 0.35
BD+68194 10.06 +0.39 +0.22 A1 V 0.36
BD+68195 10.20 +0.31 +0.01 B9 III-IV 0.37 0.31
BD+68201 9.68 +0.21 –0.06 B9 III-IV 0.27 0.24
BD+68203 10.22 +0.25 +0.13 B9 V 0.28 0.20
TE 1 11.03 +1.56 +1.37 G5 III 0.66
TE 2 12.60 +0.74 +0.27 F3 V 0.33 0.28
TE 3 11.06 +0.47 +0.37 A0 V 0.47 0.37
TE 5 10.70 +0.75 +0.07 B5 II 0.89 0.78
TE 6 12.51 +0.85 +0.71 A0 V 0.85 0.71
TE 7 11.99 +0.75 +0.65 A0 VmA5 0.75 0.65
TE 8 13.80 +0.98 +0.59 F2 V 0.63 0.58
TE 10 8.15 +1.49 +1.59 K0 III 0.48
FM C 11.28 +0.34 +0.32 A2 V 0.28 0.23
FM G 11.29 +0.63 +0.36 A8 V 0.39 0.30
FM K 10.91 +0.50 +0.36 B9.5 V 0.53 0.43
T4313-918 10.19 +0.42 B6 V 0.56
T4313-863 10.53 +0.22 B9.5 IV 0.25

HD 16907 = eclipsing binary TW Cas.
HD 17179 = V793 Cas, double-lined spectroscopic binary.

Table 1: Photometric and spectroscopic data for stars in the region of SU Cas.

For the present study we have combined the original UBV measures by Havlen (1971), Aveni & Hunter (1972), Feltz & McNamara (1976), and Turner & Evans (1984) with UBV photometry obtained by transforming the available Strömgren photometry (Feltz & McNamara, 1976; Schmidt, 1978, and Forbes, unpublished) using the relationships of Turner (1990). For a few fainter objects in the sample there are BV data from the Hipparcos/Tycho database. The data are summarized in Table 1 along with MK spectral types for the same stars obtained from the literature (see Havlen, 1971), the studies of Aveni & Hunter (1972) and Turner et al. (1985), or from new CCD spectra obtained at dispersions of 60 Å mm and 120 Å mm in November and December 2011 using the 1.8m Plaskett telescope of the Dominion Astrophysical Observatory. Stars designated as “FM” are numbered by Feltz & McNamara (1976), those as “TE” by Turner & Evans (1984), and, for completeness, stars designated as “T” are numbered from the Tycho Catalogue along with their BV data. The data for HD 23475 are from the literature (Racine, 1968), although, like many of the stars in Table 1, it appears to be unrelated to SU Cas according to the present study.

Figure 2: The reddening relation for stars near SU Cas derived from spectroscopic colour excesses. The plotted relation is described by .

Colour excesses, and , were derived for stars in Table 1 with reference to an unpublished set of intrinsic colours for early-type stars established by the lead author through a melding of published tables by Johnson (1966) and FitzGerald (1970), subsequently confirmed through applications to stars in a variety of Galactic star fields (e.g., Turner, 1989). The resulting values are plotted in Fig. 2. Intrinsic (U–B) colours for post-main-sequence late B-type stars (e.g., Johnson, 1966; FitzGerald, 1970) are particularly uncertain, which may account for some of the scatter in the diagram, notably scatter towards systematically small values of . Excess Balmer continuum emission can also account for such effects in Be stars (Schild & Romanishin, 1976). As noted by Turner (1989), the colour excess data for stars in constrained regions of sky otherwise describe reddening lines with a typical curvature term of , but with a slope ranging between extremes of +0.55 and +0.85, depending upon the line of sight along which one is viewing. The data for the majority of stars near SU Cas closely fit a reddening relation described by , provided that the three most deviant objects are omitted, similar in slope to what was found for Cyg OB2 (Turner, 1989). That relation was adopted for subsequent analysis. Reddening slope and R-value are closely correlated for nearby dust clouds in the first and second Galactic quadrants (Turner, 1989, 1996), and in the present case imply a value of , which was also adopted in the analysis.

The last result is important for establishing the distance to Alessi 95, so was examined carefully. At first glance it appears to conflict with the results of an earlier survey of the region by Turner (1976b), who found that the typical reddening law for star clusters near the Galactic longitude of SU Cas () had a slope close to 0.75–0.76, with values of averaging 3.0–3.1. In the study of Turner & Evans (1984) a value of was, in fact, adopted for the reddening corrections. Yet a re-examination of the variable-extinction data in that study (their Fig. 4) indicates that an extinction ratio of provides a much better fit to the observations than is the case for the larger value. Since the large reddening slope evident for stars near SU Cas (Fig. 2) cannot be reduced to 0.75–0.76, it appears that our adoption of for those objects is a reasonable assumption. The origin of the difference relative to the Turner (1976b) results may lie in the location of SU Cas well away from the Galactic plane (), where a localized pocket of dust has different properties from that for dust lying closer to the Galactic equator.

The reddening and distance to SU Cas and its associated dust cloud were established previously by Turner (1984) and Turner et al. (1985) using star counts and derived reddenings for stars near the Cepheid with UBV photometry, in conjunction with a technique developed by Herbst & Sawyer (1981) tied to star counts for totally opaque dust globules. Given the new information that the Cepheid lies in the core of a previously-unnoticed open cluster, the use of star counts may no longer be appropriate for the study of extinction and distance, leaving the question of the reddening for the Cepheid and cluster open to further examination.

Figure 3: Colour-colour diagram for stars in the SU Cas field, with stars lying within of the Cepheid plotted with filled symbols. The black curve is the intrinsic relation for dwarfs, while the thick gray curve represents the intrinsic relation reddened by .
Star RA(2000) DEC(2000) V B–V Star RA(2000) DEC(2000) V B–V
1 42.6032 68.9848 11.29 0.59 33 42.6618 68.8036 15.32 2.17
2 43.5207 68.8292 11.94 0.58 34 42.5644 68.7939 15.41 1.87
3 42.5635 68.8747 12.28 0.62 35 42.7140 68.8649 15.53 2.20
4 42.5214 68.9379 13.15 0.74 36 42.6204 68.8376 15.57 1.43
5 43.4562 68.8101 13.58 0.86 37 42.8804 68.8988 15.62 1.39
6 42.7422 68.9688 13.64 0.96 38 42.9933 68.9558 15.67 1.69
7 42.9819 68.9792 13.67 0.92 39 43.3421 68.7724 15.71 2.68
8 42.7272 68.8951 13.75 1.23 40 42.8359 68.8794 15.72 1.72
9 42.6903 68.7487 13.83 0.80 41 42.6393 68.8148 15.80 2.02
10 43.4705 68.8416 13.91 1.12 42 42.5626 68.7751 15.82 1.40
11 43.1982 68.7507 14.30 2.18 43 43.2426 68.7531 15.83 1.46
12 43.4667 68.9085 14.43 0.99 44 42.6391 68.9859 15.89 1.76
13 42.5669 68.8139 14.49 0.91 45 43.4950 68.9855 15.94 1.39
14 43.1307 68.8611 14.73 1.28 46 43.0456 68.9040 15.99 1.78
15 42.7000 68.9516 14.75 1.07 47 42.7820 68.8385 16.08 1.51
16 43.4772 68.7904 14.79 0.93 48 43.3109 68.8668 16.09 1.53
17 42.6767 68.8458 14.81 1.02 49 42.8790 68.7889 16.15 2.01
18 43.5128 68.9190 14.90 2.00 50 43.2876 68.8010 16.20 1.69
19 43.1200 68.9134 14.91 1.33 51 42.9461 68.9348 16.22 2.06
20 43.0688 68.8097 14.91 1.14 52 42.5290 68.8124 16.29 1.79
21 42.5517 68.8297 15.00 0.88 53 43.1040 68.9229 16.32 2.05
22 43.2084 68.9804 15.04 1.47 54 43.3733 68.8587 16.42 1.49
23 43.2299 68.8139 15.04 2.99 55 42.6019 68.9187 16.43 1.80
24 43.5362 68.8662 15.07 2.29 56 43.5272 68.8812 16.44 1.66
25 43.4419 68.7818 15.08 1.19 57 42.6220 68.9404 16.49 1.71
26 42.5198 68.7896 15.12 1.02 58 42.8224 68.8314 16.49 1.80
27 42.7201 68.7484 15.13 2.29 59 42.6265 68.9563 16.51 1.55
28 43.3182 68.7498 15.13 1.08 60 42.7998 68.9394 16.60 1.67
29 42.7834 68.9211 15.18 1.38 61 43.0472 68.7603 16.77 1.98
30 43.5239 68.9916 15.21 0.99 62 42.6304 68.7652 16.84 2.53
31 43.0970 68.7965 15.23 1.33 63 42.6872 68.7974 16.94 1.71
32 42.8776 68.8835 15.24 1.05 64 42.9295 68.8324 17.01 1.59

ARO 3 = TYC 4313-355, Sp.T. = F1 V. ARO 4, Sp.T. = A3 V.

Table 2: Abbey Ridge Observatory BV observations for stars near SU Cas.

The colours of stars in the SU Cas field are plotted in Fig. 3, with filled circles used to denote stars lying in relatively close proximity to SU Cas. Reddenings have also been derived for four additional stars lying near the Cepheid from BV data and spectral types by Aveni & Hunter (1972) along with two stars from Table 2 below, four of the six appearing to lie at similar distances to SU Cas. The derived mean reddening for the collection of 13 stars lying in close proximity to the Cepheid, and not projected against an obvious dust cloud, is s.e. ( s.d.), which also appears to apply to a few stars in the Table 1 collection (see mean reddening adopted in Fig. 3). There is noticeable differential reddening in the field according to the observations, that near SU Cas being associated with the visible dust clouds around the Cepheid. The mean reddening of the central regions of Alessi 95 can be solidly established as s.e., however, with s.e. inferred for the space reddening of a star with the observed colours of SU Cas (see Fernie, 1963).

The inferred reddening for the Cepheid is a close match to an estimate of : established by Turner, Leonard & English (1987) from published spectrophotometric KHG photometry for SU Cas in conjunction with intrinsic values established from Cepheids of well-established space reddening. The reddening also agrees reasonably well with an estimate of obtained by Kovtyukh et al. (2008) from stellar atmosphere model fitting, in this case linked to derived intrinsic colours and effective temperatures for bright stars of little to no reddening. A reddening of was derived by Laney & Caldwell (2007) from BVI photometry for SU Cas linked to a calibration based on space reddenings for Cepheids, but that included the earlier estimate of s.e. by Turner (1984). Given that SU Cas is the shortest period Cepheid in the sample of pulsators with established space reddenings, the small offset of the Laney & Caldwell (2007) reddening with the present result is presumably linked to the original underestimate of reddening for SU Cas obtained by Turner (1984).

Potential members of Alessi 95 were assembled from stars lying within the cluster boundaries: photoelectrically-observed stars (Table 1), stars in the Hipparcos/Tycho database (ESA, 1997; van Leeuwen, 2007), stars brighter than in the NOMAD database (Zacharias et al., 2005), recalibrated to the Johnson BV system using faint stars from Turner (1984) as reference standards, and stars near the Cepheid with new CCD BV observations (see below). Obvious “ringers” among the faint stars in NOMAD were omitted from the analysis, and the resulting data are plotted in Fig. 4, which represents the colour-magnitude diagram for Alessi 95 uncorrected for differential reddening or detailed membership selection. Included are a best-fitting zero-age main sequence (ZAMS, see below) and a model isochrone from Meynet, Mermilliod & Maeder (1993) for , which appears to fit the data for cluster stars and the Cepheid SU Cas reasonably well. Note that late-type dwarfs are only encountered in this direction at the distance of Alessi 95 and beyond, so the cluster cannot be less distant than implied from the ZAMS fit, for example at the distance of pc derived for the foreground dust complex (Turner & Evans, 1984).

Figure 4: Uncorrected colour-magnitude diagram for Alessi 95, with photoelectric data identified by large filled circles, stars from the Hipparcos/Tycho database by open circles, stars from the ARO survey by small filled circles, stars from NOMAD lying in the inner of the cluster by small plus signs, and SU Cas by a filled circle with bars to indicate its range of variability. The black relation is the ZAMS for , and a gray curve is a model isochrone for .

CCD observations of the central region surrounding SU Cas were made through Johnson system BV filters in September 2011 with the SBIG ST8XME camera on the Celestron 35-cm telescope of the robotic Abbey Ridge Observatory (see Lane, 2008). The observations were calibrated using previously published photoelectric UBV photometry for stars in the field (see Turner, 1984; Turner & Evans, 1984, and this paper), and are included in Fig. 4.

The reddening for individual stars was established using the reddening relation found from the spectroscopic observations (Fig. 2) through standard dereddening techniques (see Turner, 1976a, b). For stars with BV data only, colour excesses were inferred from the spatial trend of reddening across the field, except for those objects closely associated with the opaque dust clouds near the Cepheid. In all cases the B0-star reddenings averaged for spatially-adjacent stars were adopted for individually dereddened stars, then adjusted for the colour dependence of reddening to that appropriate for the inferred intrinsic colour of each object (see Fernie, 1963). In a few cases it was possible to infer an independent reddening from the spectral classification for the star. Each star was corrected for extinction using its inferred B0-star reddening in conjunction with the adopted value of .

Figure 5: Reddening and extinction-free oolour-magnitude diagram for Alessi 95, with photoelectric data identified by large filled circles, stars from the ARO survey and Hipparcos/Tycho database by small filled circles, and SU Cas as in Fig. 4. Open circles denote the 6 stars from Table 1 that may be outlying cluster members. The black relation is the ZAMS for , and the gray curve is a model isochrone for .

The resulting data are plotted in Fig. 5 along with similarly-derived data for six stars in Table 1 that appear to share comparable space motions and parallaxes with SU Cas. Observed radial velocities (see Turner & Evans, 1984; Turner et al., 1985), proper motions (van Leeuwen, 2007), and parallaxes (van Leeuwen, 2007) were used to identify only bona fide potential outlying cluster members on the basis of similarity of the values to those for SU Cas.

Hipparcos Star
(mas) (mas)
11633 BD+68 170 2.31 1.46
12434 HD 16228 2.80 1.23
12567 HD 16393 3.03 0.52
12924 HD 16841 3.08 1.01
13138 BD+70 205 1.04 1.02
13208 HD 17327 0.98 0.77
13219 BD+69 181 1.82 1.20
13367 SU Cas 2.53 0.32
13465 BD+68 201 0.89 1.34
13595 BD+69 186 0.82 1.47
13728 HD 17929 2.84 0.64
13956 BD+69 189 2.36 1.40
14442 BD+70 224 0.60 1.10
14483 BD+67 243 –0.97 1.99
14714 HD 19287 1.02 1.32
15138 HD 19856 1.13 1.09
15959 HD 20710 4.19 0.61
16633 HD 21725 0.86 1.25
1
Table 3: Hipparcos parallax data for members and potential outlying members of Alessi 95

The reddening for individual members of Alessi 95 is well enough established for 26 likely ZAMS members of the cluster to derive a mean intrinsic distance modulus of s.e. ( s.d.). The zero-age main sequence (ZAMS) adopted here is that of Turner (1976a, 1979), and the fit corresponds to a distance of pc, with the cited uncertainty representing the standard error of the mean. A model isochrone for from Meynet et al. (1993) fits the data reasonably well, with a likely uncertainty in no larger than . It is possible to use alternate evolutionary isochrones from the literature, but they do not match the adopted ZAMS nearly as well. The isochrone fit for Alessi 95 is not ideal for SU Cas, but that problem could be resolved by accounting for the opacity effects of CNO mixing in the envelopes of post-supergiant stars (see Xu & Li, 2004). A more typical solution to the problem of a compressed blue loop for core helium-burning stars is to adopt a metallicity for the isochrone that is smaller than the solar value, but that does not appear to be justified in the case of Alessi 95, given that the derived metallicity of SU Cas (and two associated stars) from stellar atmosphere models is close to solar ([Fe/H] = –0.12, +0.02, –0.01, and +0.06 according to Kovtyukh et al. (1996); Usenko et al. (2001); Andrievsky et al. (2002); Luck et al. (2008), respectively).

Three of the bright members of Alessi 95, as well as 15 other stars lying within a few degrees of SU Cas sharing similar space motions (proper motions and in a few cases radial velocities) with the Cepheid and with colours and magnitudes consistent with the isochrone in Fig. 4, are catalogued in the Hipparcos catalogue (van Leeuwen, 2007). The stars are collected in Table 3, along with their cited parallaxes and uncertainties. The weighted mean parallax for the group is mas, corresponding to a distance of pc. An attempt was also made to include the less precise parallaxes from the Tycho catalogue (ESA, 1997) in the result. A further fifteen stars were considered in such fashion, but the resulting mean parallax and distance remained unaffected, since the extra stars add negligible weight to the overall solution because of their large parallax uncertainties. In both cases the parallax solution is in excellent agreement with the cluster distance of pc derived from ZAMS fitting.

A further consistency check on the results was made using JHK photometry (Cutri et al., 2003) from the Two Micron All Sky Survey (2MASS, Skrutskie et al., 2006) for Galactic star fields. Stars lying within of the centre of Alessi 95 with proper motions similar to that of SU Cas are plotted in colour-colour and colour-magnitude diagrams in Fig. 6 in the manner adopted by Turner (2011). Also included are similar data for the stars from Table 1 and Fig. 5 selected on the basis of comparable space motion with SU Cas. Most of the scatter in the observations can be attributed to photometric uncertainties, yet the data are a reasonably close match to the results inferred from the UBV analysis, namely the implied reddening and distance modulus.

Figure 6: JHK colour-colour diagram (upper) and colour-magnitude diagram (lower) for stars in Alessi 95 (filled circles) and outlying stars (open circles), indicated to be potential cluster members from proper motion data. SU Cas is denoted by a star symbol. The black relation in the upper diagram is the intrinsic relation for dwarfs, while the gray relation corresponds to a reddening of . The black relation in the lower diagram is the ZAMS for , and the gray curve is a model isochrone for .

A program was also completed in January 2012 to obtain JHK photometry of greater precision for the field of Alessi 95 using queue observing with the near-infrared imager (CPAPIR) of l’Observatoire du Mont-Mégantic (OMM Artigau et al., 2010). The details of that study, to be presented elsewhere, provide much stronger confirmation of the optical results than is the case for the less precise 2MASS data, and also provide information on the extreme lower end of the cluster main sequence.

The nuclear and coronal radii for Alessi 95 implied by its distance derived from ZAMS fitting are 3 pc and pc, respectively. Both values are reasonable, although a larger tidal radius is expected, which would explain the presence of outlying cluster members a few degrees from SU Cas.

3 Su Cas as a Member of Alessi 95

In the studies by Schmidt (1978) and Turner & Evans (1984) of stars associated with the dust complexes near SU Cas it was noted that the dust clouds lie at different distances. The two main clouds at the declination of SU Cas and south of it are at distances of pc and pc according to the Turner & Evans (1984) study. SU Cas was assumed to lie at the distance of the former, according to a perceived connection on Palomar Observatory Sky Survey (POSS) plates of the SU Cas dust complex with that associated with HD 16893 and HD 17443, which were calculated to be 258 pc distant.

The deeper POSS images used for the production of Fig. 1 indicate that such an assumption cannot be correct. The reflection nebulae illuminated by SU Cas that lie south of the Cepheid display no association with the opaque dust cloud east of it that continues further to the northeast. Strands of the same opaque cloud are seen to the west and south of SU Cas, connecting with the clouds illuminated by HD 16893 and HD 17443, but the main cloud east of SU Cas displays no evidence for associated reflection nebulosity, so must lie foreground to the Cepheid. The true geometry of the stars and dust is revealed by those members of Alessi 95 that, from their large reddenings, must be viewed through the dust extinction of the main cloud. SU Cas and Alessi 95 therefore lie beyond the main dust complex located at 258 pc. Indeed, the derived distance of pc to Alessi 95 agrees closely with the previous estimate (Turner & Evans, 1984) for the distance to the further dust complex in the field.

The derived luminosity for SU Cas as a member of Alessi 95, including the uncertainty in its field reddening, is s.e., where the Cepheid’s magnitude (Berdnikov, 2007) has been adjusted for contamination by an unseen B-type companion 4.2 magnitudes fainter (Evans & Arellano Ferro, 1987). The result is more than a magnitude more luminous than expected for a classical Cepheid with a mean period of days, as used in studies of the star’s period changes (Berdnikov et al., 1997, 2003; Turner, Abdel-Sabour Abdel-Latif & Berdnikov, 2006). The Cepheid must therefore be an overtone pulsator, as argued previously (e.g., Gieren, 1976, 1982). According to the empirical relationship between fundamental mode and first overtone pulsation periods established for double-mode Cepheids by Szabados (1988), the undetected mean period for fundamental mode pulsation in SU Cas must be days.

An independent distance estimate for SU Cas is possible from its radius and inferred mean effective temperature, using the infrared surface brightness variant of the Baade-Wesselink method, as noted by Storm et al. (2011). The estimated distance to SU Cas in that study is pc for a pulsation period of . With the revised space reddening found here for SU Cas and a local ratio of total-to-selective extinction of , the derived distance becomes pc for fundamental mode pulsation (). The distance estimates are not completely independent, but the methodologies are. The close agreement in the pulsation parallax, trigonometric parallax, and cluster parallax estimates for the distance to Alessi 95 and SU Cas —  pc, pc, and pc, respectively, all of which agree to within their derived uncertainties — provides strong confirmation of their validity.

The implied mean radius of SU Cas according to the Cepheid period-radius relation of Turner et al. (2010), which is tied to the almost identical slopes for the Cepheid period-radius relation in studies by Gieren, Barnes & Moffett (1989), Laney & Stobie (1995), Gieren, Fouqué & Gómez (1998), and Turner & Burke (2002), is 25.0 . By comparison, the surface brightness technique yields a mean radius of , while an independent Baade-Wesselink analysis using infrared colours by Milone et al. (1999) produced an estimate of . The last study also summarizes previous estimates for the mean radius of SU Cas derived from variants of the Baade-Wesselink method, most of which lie in the range 30–45 . Systematic effects cannot be discounted, given the small amplitude of the light variations in SU Cas and the fact that Milone et al. (1999) adopted a projection factor of in their study. Laney & Joner (2009) find a value of to be more suitable for SU Cas, which would reduce the Milone et al. (1999) value to . The VJK photometry used by Laney & Joner (2009) leads to a mean radius of for SU Cas, while Turner & Burke (2002) obtained a radius of using a Baade-Wesselink analysis tied to KHG photometry. The last three estimates are closer to the value predicted by the Cepheid period-radius relation, and it may be that the star’s small pulsation amplitude and contamination by its B-type companion limit further improvement.

With the period of fundamental mode pulsation in SU Cas indicated by its membership in Alessi 95, one can estimate independently the age of the Cepheid from existing period-age relations. A model-based relationship derived by Bono et al. (2005) yields an age of for a solar metallicity Cepheid with , while a relationship by Efremov & Elmegreen (1998) calibrated by isochrone fits to open clusters yields a similar age of . Both cited relationships display a dispersion in of , so are consistent with the cluster age inferred from the model isochrones of Meynet et al. (1993). Additionally, the implied age of for SU Cas from its membership in Alessi 95 provides a key point at the short-period end of a semi-empirical period-age relationship for cluster Cepheids developed by Turner (2012), where again the dispersion is no larger than in and the relationship is generated by isochrone fits to clusters containing Galactic Cepheids.

The luminosity of SU Cas inferred from cluster membership, namely , can be compared with a value of predicted from its inferred radius and effective temperature via the methodology described by Turner & Burke (2002) and Turner et al. (2010). The offset from the empirical estimate is comparable to the offsets observed for other cluster Cepheids (Turner, 2010), and can be partially explained by the nature of SU Cas: a small-amplitude Cepheid lying near the high temperature side of the instability strip, as also argued by its overtone pulsation. SU Cas has an unseen B9.5 V companion detected by IUE (Evans & Arellano Ferro, 1987), and the luminosity inferred for the Cepheid according to the implied magnitude difference between SU Cas and the B-star in ultraviolet spectra is (Evans & Arellano Ferro, 1987), closely coincident with the result from cluster membership. The companion, which may also be an Ap star (Turner, 2003), has otherwise only a small effect on the overall visual brightness and colours of SU Cas.

Confirmation of the location of SU Cas towards the blue edge of the Cepheid instability strip is provided by its observed rate of period change of +0.024 s yr (Berdnikov et al., 1997, 2003; Turner et al., 2006). That implies a rate of evolution for the Cepheid that is more than twice as rapid as what is typical of fundamental mode pulsators with periods of near the centre of the instability strip (Turner et al., 2006). The consistency in the implied parameters for SU Cas found from such diverse observational material provides further validation of the present results.

4 Discussion

This first detailed photometric and spectroscopic study of Alessi 95, the sparse open cluster surrounding the Cepheid SU Cas, produces empirical estimates for the reddening and luminosity of a bona fide Cepheid calibrator. Estimates for the distance to SU Cas and Alessi 95 from ZAMS fitting, Hipparcos parallaxes (van Leeuwen, 2007), and the Cepheid’s pulsation parallax (Storm et al., 2011, adjusted here) agree closely to within a few percent, to our knowledge the first such instance of a tight consensus in distance estimates by these diverse methods. Future improvement to the cluster ZAMS fit might be possible, for example through a more detailed analysis that accounts implicitly for the metallicity of SU Cas and Alessi 95 members. That affects ZAMS fitting through small offsets in the zero-point, which is currently calibrated for solar metallicity stars. Given present knowledge of the near-solar chemical composition for Alessi 95 stars (Usenko et al., 2001), however, only a very minor improvement would be expected.

The inferred field reddening of found here for SU Cas agrees reasonably well with other independent estimates (Turner et al., 1987; Laney & Caldwell, 2007; Kovtyukh et al., 2008), and the effective temperature of 6620K for SU Cas inferred from its colour via the semi-empirical technique described by Turner & Burke (2002) and Turner et al. (2010) is only slightly greater than the values obtained by Usenko et al. (2001) from stellar atmosphere models. Any discrepancies between the present results and those of previous studies appear to be minor, except for the inferred luminosity of s.e., which differs from that found in the earlier study by Turner & Evans (1984), primarily because of an erroneous selection of reflection nebulosity stars associated with the Cepheid in that paper. Future work may improve the situation, since Hipparcos parallaxes, pulsation parallaxes, and cluster parallaxes are all susceptible to systematic effects that are the subject of ongoing study. It should be evident, however, that there is no longer a need to rely on the Cepheid’s membership in Cas R2 to derive its intrinsic parameters (e.g., Turner & Evans, 1984; Usenko et al., 2001; Turner, 2010).

Acknowledgements

This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. The authors gratefully acknowledge the use of data products from the SAO/NASA Astrophysics Data System (ADS) in this study, and are indebted to the Dominion Astrophysical Observatory for the generous allotment of observing time for the new spectroscopic results presented here and to Noel Carboni for the creation of Fig. 1. We also thank the referee, Clifton Laney, for helpful suggestions on the original manuscript. WPG gratefully acknowledges support from the Chilean Center for Astrophysics FONDAP 15010003 and the BASAL Centro de Astrofisica y Tecnologias Afines (CATA) PFB-06/2007.

Footnotes

  1. footnotetext: BD+68 201 = FM-A.

References

  1. Alessi B. S., 2006, unpublished data
  2. Alessi B. S., Moitinho A., Dias W. S., 2003, A&A, 410, 565
  3. Andrievsky S. M., Kovtyukh V. V., Luck R. E., et al., 2002, A&A, 381, 32
  4. Artigau É. M., Lamontagne R., Doyon R., Malo L., 2010, in Silva D. R., Peck A. B. & Soifer B. T., eds., Observatory Operations: Strategies, Processes, and Systems III, Proceedings of the SPIE, 7737, pp. 1O 1-7
  5. Aveni A. F., Hunter J. H., 1972, AJ, 77, 17
  6. Berdnikov L. N., 2007, http://www.sai.msu.ru/groups/ cluster/CEP/PHE
  7. Berdnikov L. N., Ignatova V. V., Pastukhova E. N., Turner D. G., 1997, AstL, 23, 177
  8. Berdnikov L. N., Mattei J. A., Beck S. J., 2003, JAAVSO, 31, 146
  9. Bono G., Marconi M., Cassisi S., et al., 2005, ApJ, 621, 966
  10. Cutri R. M. et al., 2003, The IRSA 2MASS All-Sky Point Source Catalog of Point Sources, NASA/IPAC Infrared Science Archive
  11. Efremov Yu. N., Elmegreen B. G., 1998, MNRAS, 299, 588
  12. ESA, 1997, The Hipparcos and Tycho Catalogues, ESA SP-1200
  13. Evans N. R., Arellano Ferro A., 1987, in Stellar Pulsation, Springer-Verlag, Berlin, Lecture Notes in Physics, 274, p. 183
  14. Feltz K. A., Jr., McNamara D. H., 1976, PASP, 88, 699
  15. Fernie J. D., 1963, AJ, 68, 780
  16. FitzGerald M. P., 1970, A&A, 4, 234
  17. Gieren W., 1976, A&A, 47, 211
  18. Gieren W., 1982, PASP, 94, 960
  19. Gieren W. P., Barnes T. G., III, Moffett T. J., 1989, ApJ, 342, 467
  20. Gieren W. P., Fouqué P., Gómez M., 1998, ApJ, 496, 17
  21. Johnson H. L., 1966, ARA&A, 4, 193
  22. Kovtyukh V. V., Andrievsky S. M., Usenko I. A., Klochkova V. G., 1996, A&A, 316, 155
  23. Kovtyukh V. V., Soubiran C., Luck R. E., et al., 2008, MNRAS, 389, 1336
  24. Kronberger M., Teutsch P., Alessi B., et al., 2006, A&A, 447, 921
  25. Havlen R. J., 1971, Ph.D. Thesis, Univ. Arizona
  26. Herbst W., Sawyer D. L., 1981, ApJ, 243, 935
  27. Lane D. J., 2008, JAAVSO, 36, 143
  28. Laney C. D., Stobie R. S., 1995, MNRAS, 274, 337
  29. Laney C. D., Caldwell J. A. R., 2007, MNRAS, 377, 147
  30. Laney C. D., Joner M. D., 2009, in Guzik J. A. & Bradley P. A., eds., Stellar Pulsation: Challenges for Theory and Observation, Melville, New York, AIP Conf. Proc., 1170, p. 93
  31. Luck R. E., Andrievsky S. M., Fokin A., Kovtyukh V. V., 2008, AJ, 136, 98
  32. Meynet G., Mermilliod J.-C., Maeder A., 1993, A&AS, 98, 477
  33. Milone E. F., Wilson W. J. F., Volk K., 1999, AJ, 118, 3016
  34. Racine R., 1968, AJ, 83, 960
  35. Racine R., van den Bergh S., 1970, in Becker W. & Kontopoulos G. I., eds., The Spiral Structure of our Galaxy, Reidel, Dordrecht, IAU Symp., 38, p. 219
  36. Schild R., Romanishin W., 1976, ApJ, 204, 493
  37. Schmidt E. G., 1978, AJ, 73, 588
  38. Skrutskie M. F. et al., 2006, AJ, 131, 1163
  39. Storm J., Gieren W., Fouqué P., et al., 2011, A&A, 534, A94
  40. Szabados L., 1988, in Kovács G., Szabados L. & Szeidl B., eds., Multimode Stellar Pulsations, Konkoly Obs., Budapest, p. 1
  41. Turner D. G., 1976a, AJ, 81, 97
  42. Turner D. G., 1976b, AJ, 81, 1125
  43. Turner D. G., 1979, PASP, 91, 642
  44. Turner D. G., 1984, JRASC, 78, 229
  45. Turner D. G., 1989, AJ, 98, 2300
  46. Turner D. G., 1990, PASP, 102, 1331
  47. Turner D. G., 1996, in Milone E. F. & Mermilliod J.-C., eds., The Origins, Evolution, and Destinies of Binary Stars in Clusters, ASPC, 90, p. 382
  48. Turner D. G., 2003, in Gray R. O., Corbally C. J & Philip A. G. D., eds., The Garrison Festschrift, L. Davis Press, Schenectady, N.Y., p. 101
  49. Turner D. G., 2010, Ap&SS, 326, 219
  50. Turner D. G., 2011, RMxAA, 47, 127
  51. Turner D. G., 2012, JAAVSO, 40, in press
  52. Turner D. G., Evans N. R., 1984, ApJ, 283, 254
  53. Turner D. G., Burke J. F., 2002, AJ, 124, 2931
  54. Turner D. G., Forbes D. W., Lyons R. W., Havlen R. J., 1985, in Madore B. F., ed., Cepheids: Theory and Observations, IAU Colloq. 82, p. 95
  55. Turner D. G., Leonard P. J. T., English D. A., 1987, AJ, 93, 368
  56. Turner D. G., Abdel-Sabour Abdel-Latif M., Berdnikov L. N., 2006, PASP, 118, 410
  57. Turner D. G., Majaess D. J., Lane D. J., et al., 2010, Odessa Astron. Publ., 23, 119
  58. Usenko I. A., Kovtyukh V. V., Klochkova V. G., et al., 2001, A&A, 367, 831
  59. van den Bergh S., 1957, ApJ, 126, 323
  60. van den Bergh S., 1966, AJ, 71, 990
  61. van Leeuwen F., 2007, Hipparcos, the New Reduction of the Raw Data, Springer, Heidelberg, Astrophysics and Space Science Library, 370
  62. Xu H. Y., Li Y., 2004, A&A, 418, 213
  63. Zacharias N., Monet D., Levine S., Urban S., Gaume R., Wycoff G., 2005, The Naval Observatory Merged Astrometric Dataset (NOMAD), BAAS, 36, 1418
264058
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
Edit
-  
Unpublish
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel
Comments 0
Request comment
""
The feedback must be of minumum 40 characters
Add comment
Cancel
Loading ...

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description