Radial-velocity curves for RR Lyrae stars in the globular clusters M5 and M92 obtained using synthetic spectra cross-correlation templates

Storm, J.; Carney, Bruce W.; Latham, David W.; Davis, R. J.; Laird, John B.

doi:10.1086/132974

Cited by 8 publications

(7 citation statements)

References 14 publications

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“…These were -128.1 for M92-Vl and -132.7 km s-1 for M92-6. The vy determined by Storm et al (1992) for M92-Vl is -125.4 km s-1 , in good agreement with our determination, while the systemic radial velocity for M92 compiled by Webbink (1981) is -120.5 with a dispersion of 6.7 km s-1 . The M5 vr velocities of Cohen & Gordon (1987) lie very close to the systemic velocity of M5 given by Webbink.…”

Section: Observational Materials For the Globular Cluster Rr L Yrae Vasupporting

confidence: 89%

“…Cohen & Gordon (1987) began the application of the Baade-Wesselink method to globular cluster stars, and that work is continued here. In the interim Liu & Janes (1990) observed four stars in M4 using the infrared Baade-Wesselink method, while Storm et al (1992) are working on two stars in M5 and two in M92. We continue our program by providing in this paper an infrared Baade-Wesselink analysis for two RR Lyrae variables in M92 and four in M5.…”

Section: Introductionmentioning

confidence: 99%

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The Baade-Wesselink method applied to RR Lyrae variables in the globular clusters M5 and M92

Cohen¹

1992

ApJ

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An infrared Baade-Wesselink analysis is given for two RR Lyrae variables in the extremely metal-poor globular cluster M92 and four in the intermediate metallicity cluster M5. The method of analysis relies on the theoretical model atmospheres of Kurucz and on the absolute flux calibration of observed V-and Kmagnitudes. The best results are obtained with V-K colors to obtain T.rr and K-magnitudes to deduce absolute fluxes. We obtain a distance to M5 of 6.9 ± 0.45 kpc and to M92 of 7.85 ± 0.45 kpc, with a 0.3 kpc additional systematic uncertainty. These results are in excellent agreement with the previously published distances, based on matching the globular cluster main sequence to that defined by the field subdwarfs of known distance. With these distances we obtain an absolute mean magnitude corrected for reddening, Mi, of 0.86 ± 0.14 mag for the M5 RR Lyrae variables, while Mi= 0.62 ± 0.11 for the M92 RR Lyrae variables. The globular cluster RR Lyrae stars appear to behave just like the field RR Lyrae stars. They obey the same (Mv)-[Fe/HJ relationship as do the field stars, and the same (MK)-period relationship. Previous work which assumed the two groups of stars to behave identically is thus shown to be correct.

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Section: Observational Materials For the Globular Cluster Rr L Yrae Vasupporting

confidence: 89%

Section: Introductionmentioning

confidence: 99%

The Baade-Wesselink method applied to RR Lyrae variables in the globular clusters M5 and M92

Cohen¹

1992

ApJ

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“…Note that the comparison between the K−band mean magnitude of RR Lyrae stars and predicted K−band ZAHB brightness at log T e = 3.85 appears as a very promising approach, since in this band the evolutionary effects also imply a change in effective temperature (Bono et al 2001). The seventh column of Table 4 gives the distance to M92 estimated using the near-infrared Baade-Wesselink (BW) method for two cluster RR Lyrae stars observed by Cohen (1992) and by Storm et al (1994). The last column in Table 4 lists the distance modulus to M92 using the empirical calibration of the luminosity of the RGB tip recently provided by Bellazzini et al (2004) and shortly discussed in Sect.…”

Section: Discussionmentioning

confidence: 99%

“…During the last few years, the sample of RR Lyrae stars has been investigated more in the optical than in the NIR bands Cohen 1992;Cohen & Matthews 1992;Storm, Carney & Latham 1992, hereinafter SCL;Kopacki 2001;Piersimoni et al 2003;Tuairisg et al 2003). In particular, NIR observations for 3 RR Lyrae stars have been collected by Cohen (1992) and by Storm, Carney, & Latham (1994) to estimate the distance to M92 using the Baade-Wesselink method.…”

Section: The Clustermentioning

confidence: 99%

Near-Infrared Observations of RR Lyrae Variables in Galactic Globular Clusters. I. The Case of M92

et al. 2005

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We present near-infrared J,H, and K-band time series observations of the Galactic Globular Cluster (GGC) M92. On the basis of these data, we derived well-sampled light curves for eleven out of the seventeen cluster RR Lyrae variables, and in turn, accurate mean near-infrared (NIR) magnitudes. The comparison between predicted and empirical slopes of NIR Period-Luminosity (PL) relations indicates a very good agreement. Cluster distance determinations based on independent theoretical NIR P L relations present uncertainties smaller than 5% and agree quite well with recent distance estimates based on different distance indicators. We also obtained accurate and deep NIR color-magnitude diagrams (CMDs) ranging from the tip of the Red Giant Branch (RGB) down to the Main Sequence Turn-Off. We detected the RGB bump and the NIR luminosities of this evolutionary feature are, within theoretical and empirical uncertainties, in good agreement with each other.

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“…Carney et al (1992) presented BV photometry and light curves of seven RR Lyrae stars in the hope of using two of them (catalogue variables V1 and V3) for distance determination using Baade–Wesselink (BW) analysis. Cohen & Matthews (1992) followed this up with photometry in V and i for five RR Lyrae stars, updating periods and deriving mean magnitudes again for BW analysis, as did Storm et al (1992) using K ‐band light curves. A search for erupting dwarf novae (DNe) in M92 was initiated by Shara, Bergeron & Moffat (1994).…”

Section: Introductionmentioning

confidence: 99%

TRIFFID observations of the cores of the three globular clusters M15, M92 and NGC 6712

Tuairisg

Butler

Shearer

et al. 2003

Monthly Notices of the Royal Astronomical Society

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We present the results of TRIFFID simultaneous V‐ and B‐band observations of the cores of the globular clusters M15, M92 and NGC 6712. A variability search of their dense centres was made feasible through performing post‐exposure image sharpening on the images, increasing the image resolution by a factor of ∼2. The isis implementation of the image subtraction technique developed by Alard & Lupton was then used to detect flux variations in our image sets. We have obtained periods for all observable variables (in our field of view) in NGC 6712 and we have found two new RR Lyrae variables (an RRab and an RRc). We have confirmed three variables in our field of view of the M92. For M15, we detect 48 variables in our field of view, 23 of which are new discoveries. We obtain periods and amplitudes for all variables and classify new ones based on the light‐curve shape, the most significant period and the mean magnitude in the V band. Among the detected RR Lyrae we find 19 RRc, 12 RRab and two RRd types. In the subsequent analysis we find a marked increase in RRc over RRab variables in the core. In a refined procedure to search for fainter objects we find no dwarf novae in our field of view of M15. Simulations performed on the data set to quantify our sensitivity to such objects indicate that an upper limit of 10 dwarf novae (at 92 per cent probability) exist in our field of view. The implications this result has on globular clusters are discussed.

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Radial-velocity curves for RR Lyrae stars in the globular clusters M5 and M92 obtained using synthetic spectra cross-correlation templates

Cited by 8 publications

References 14 publications

The Baade-Wesselink method applied to RR Lyrae variables in the globular clusters M5 and M92

The Baade-Wesselink method applied to RR Lyrae variables in the globular clusters M5 and M92

Near-Infrared Observations of RR Lyrae Variables in Galactic Globular Clusters. I. The Case of M92

TRIFFID observations of the cores of the three globular clusters M15, M92 and NGC 6712

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