Cepheid period-luminosity relations in K, H, J and V

Laney, C. D.; Stobie, R. S.

doi:10.1093/mnras/266.2.441

Cited by 135 publications

(177 citation statements)

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“…We also note that the models yield a difference of distance moduli between SMC and LMC of ∼0.45, in good agreement with previous determinations based on Cepheids (Laney & Stobie 1994;Udalski et al 1999c), RR Lyr or Red Clump stars (cf. Udalski et al 1999c;Udalski 2000).…”

Section: P -W I Diagramsupporting

confidence: 91%

“…We adopt the dereddened data provided by the OGLE2 catalog, with different reddening corrections for each fields (see Udalski et al 1999b for details) and the same distance modulus µ 0 = 18.94 as used in Alibert et al (1999). This value, suggested by Laney & Stobie (1994), yields general agreement between models and various observations for fundamental pulsators (cf. Alibert et al 1999).…”

Section: Smc Cepheids: VI -Bandssupporting

confidence: 78%

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Period -magnitude relationships inBVIJHK-bands for fundamental mode and first overtone Cepheids

Baraffe

Alibert

2001

A&A

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Abstract. We present theoretical period -magnitude relationships for Cepheids in different filters for fundamental and first overtone pulsators, completing the work by Alibert et al. (1999). The results are provided for different metallicities characteristic of the Magellanic Clouds and the Milky Way. In contrast to the fundamental mode, we find a small metallicity effect on the period -luminosity relationship for the first overtone, due to the sensitivity of the period ratio P1/P0 with metallicity. Comparison is made with observations from OGLE and EROS in the Small and Large Magellanic Clouds. We emphasize the constraint on theoretical predictions provided by the combination of both fundamental and first overtone observed sequences. We obtain excellent agreement between models and data in a log P -WI (Wesenheit index) diagram for a distance modulus for the LMC µ0 = 18.60 -18.70. We analyse the uncertainties of the fundamental period -magnitude relationships and the consequences on distance determination. We show that an arbitrary shift of the instability strip by 350 K in T eff yields up to 0.45 mag effect on MV at a given period, whereas the effect is less than 0.1 mag in the K-band. Using recent near-IR observations in the Large Magellanic Cloud and our P -MK relationship, we derive a distance modulus for the LMC in agreement with the value based on WI data.

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Section: P -W I Diagramsupporting

confidence: 91%

Section: Smc Cepheids: VI -Bandssupporting

confidence: 78%

Period -magnitude relationships inBVIJHK-bands for fundamental mode and first overtone Cepheids

Baraffe

Alibert

2001

A&A

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“…Combining these with the dereddened mean magnitudes for 45 LMC and 47 SMC Cepheids with VJHK photometry enables period-luminosity relations in each colour to be derived with effective "distance moduli" for the LMC and SMC. Corrected for the effects of mean difference in temperature at a given period and for the differences in blanketing between galactic and Cloud Cepheids (as in Laney & Stobie 1994), we find that the corrected VJHK moduli are in agreement, with means of 18.58±0.04 for the LMC and 19.00±0.04 for the SMC. These mean values are in remarkably good agreement with the moduli of 18.53 and 18.94 we found using the galactic Cepheids in clusters and associations together with the same sample of Cloud Cepheids (Pleiades modulus 5.57).…”

mentioning

confidence: 52%

Cepheid Radii and Distances

Laney

Stobie

1995

International Astronomical Union Colloquium

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Laney & Stobie (1995) (LS95) have determined Baade-Wesselink radii for 49 galactic Cepheids using BVRI and JHK photometry. Four of the possible magnitude-colour combinations were studied in detail -namely, (V,B-V), (V,VIc), (K,V-K) and (K,J-K). In that paper and in the present note we have used the maximum likelihood method of Balona (1977) as recently modified to allow for the nonlinear effects of the non-negligible radius excursions of Cepheids.One major advantage of infrared photometry is that the light variation at K is dominated by the change in surface area, unlike the light variation at V which is dominated by temperature changes. Another is that (as shown both empirically and by model atmospheres) one may use a J-K or V-K colour index to calculate the surface brightness at K without having to worry very much about the effects of varying surface gravity or Doppler broadening velocity, while the same is definitely not true when optical colour indices are used to calculate the surface brightness at V.From radius displacement curves it is clear that the systematic and random errors are least in the case of the infrared solutions, (K,V-K) and (K,J-K). (V,B-V) and (V,V-Ic) solutions have large systematic and random errors. Furthermore, "optical" radius determinations appear quite sensitive to whether the phase of the ascending branch is excluded from the solution. "Infrared" solutions show no such effect.The most accurate period-radius relation was derived by averaging the (K,V-K) and (K,J-K) radius solutions. (V,B-V) and (V,V-I) solutions gave systematically incorrect radius determinations because of the effects of surface gravity and microturbulence variations throughout the pulsation cycle. (V,VRj) radius solutions (calculated for about half of our sample) showed systematic errors essentially identical to those seen in (V,V-Ic) solutions.Given the availability of radial velocities contemporaneous with our JHK data for LMC and SMC Cepheids, we have calculated "infrared" radii for as many Cepheids as possible, despite the limited quality and limited precision of the data compared to our galactic sample. Contemporaneous radial velocities were available in the literature. Radius solutions were considered successful only if the surface brightness coefficients were within 0.6 of the expected value at a given period. No solutions for Cepheids with periods longer than 100 days were successful. For 5 LMC and 4 SMC Cepheids (HV 12815, 879, 2338, 2827, 5497, 837, 824, 11157, and 829), radii could be determined, and the adopted radii are plotted in Fig. 1, together with our "adopted" galactic Cepheid radii. The LMC and SMC Cepheid radii show no systematic difference from the galactic Cepheid 254 terms of use, available at https://www.cambridge.org/core/terms. https://doi

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“…Nandy published several papers on reddening laws in different Galactic directions (e.g., Nandy 1968) and came to the general conclusion that the form of the reddening law was well approximated by ␦m abs F Ϫ1 over the wavelength range 4000 -10000 Å, and was independent of direction to first order. Taking the extinction in the V band to be 3.20E(B Ϫ V ) (e.g., Laney & Stobie 1994) then leads to an extinction coefficient of 2.77E(B Ϫ V ) for the R band. The maps of Burstein & Heiles (1982) do not extend inward of Galactic latitudes of 10Њ; however, the Pyxis cluster at l ϭ 261$3, b ϭ 7$0, lies in a region of lower than average Galactic absorption with only slowly varying contours of extinction.…”

Section: Schmidt (1976) Gives E(rmentioning

confidence: 99%

The Pyxis Cluster: A Newly Identified Galactic Globular Cluster

Irwin

Demers

Kunkel

1995

ApJ

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One of the ''interesting'' objects identified by Weinberger during an eyeball search of sky survey plates for planetary nebulae is a previously unrecognized distant Galactic halo globular cluster. Deep B, R, and I CCD frames of the object to R ϭ 23 reveal it to be a cluster of stars some 2Ј in core size, with a well-defined main sequence with a turnoff at R ϭ 22 and a sparsely populated subgiant branch leading to a stubby red horizontal branch at R ϭ 18.7. With a reddening-corrected distance modulus of 18.0, corresponding to a distance of 40 kpc, the Pyxis globular cluster is the latest addition to an exclusive club of distant Galactic satellites. Pyxis is similar in morphological appearance to other outer halo globular clusters and lies tantalizingly close to the plane of the Magellanic Clouds orbit (Jones and coworkers), suggesting it might be a detached cluster of this system.

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Cepheid period-luminosity relations in K, H, J and V

Cited by 135 publications

References 0 publications

Period -magnitude relationships inBVIJHK-bands for fundamental mode and first overtone Cepheids

Period -magnitude relationships inBVIJHK-bands for fundamental mode and first overtone Cepheids

Cepheid Radii and Distances

The Pyxis Cluster: A Newly Identified Galactic Globular Cluster

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