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J/MNRAS/434/1220   Vi light curves of NGC6333 variables  (Arellano Ferro+, 2013)

A detailed census of variable stars in the globular cluster NGC 6333 (M9) from CCD differential photometry. Arellano Ferro A., Bramich D.M., Figuera Jaimes R., Giridhar S., Kains N., Kuppuswamy K., Jorgensen U.G., Alsubai K.A., Andersen J.M., Bozza V., Browne P., Calchi Novati S., Damerdji Y., Diehl C., Dominik M., Dreizler S., Elyiv A., Giannini E., Harpsoe K., Hessman F.V., Hinse T.C., Hundertmark M., Juncher D., Kerins E., Korhonen H., Liebig C., Mancini L., Mathiasen M., Penny M.T., Rabus M., Rahvar S., Ricci D., Scarpetta G., Skottfelt J., Snodgrass C., Southworth J., Surdej J., Tregloan-Reed J., Vilela C., Wertz O. <Mon. Not. R. Astron. Soc. 434, 1220 (2013)> =2013MNRAS.434.1220A
ADC_Keywords: Clusters, globular ; Stars, variable ; Photometry, CCD Keywords: stars: variables: general - stars: variable: RR Lyrae - globular clusters: individual: NGC 6333 Abstract: We report CCD V and I time series photometry of the globular cluster NGC 6333 (M9). The technique of difference image analysis has been used, which enables photometric precision better than 0.05mag for stars brighter than V∼19.0mag, even in the crowded central regions of the cluster. The high photometric precision has resulted in the discovery of two new RRc stars, three eclipsing binaries, seven long-term variables and one field RRab star behind the cluster. A detailed identification chart and equatorial coordinates are given for all the variable stars in the field of our images of the cluster. Our data together with the literature V-data obtained in 1994 and 1995 allowed us to refine considerably the periods for all RR Lyrae stars. The nature of the new variables is discussed. We argue that variable V12 is a cluster member and an Anomalous Cepheid. Secular period variations, double-mode pulsations and/or the Blazhko-like modulations in some RRc variables are addressed. Through the light-curve Fourier decomposition of 12 RR Lyrae stars we have calculated a mean metallicity of [Fe/H]ZW=-1.70±0.01(statistical)±0.14(systematic) or [Fe/H]UVES=-1.67±0.01(statistical)±0.19(systematic). Absolute magnitudes, radii and masses are also estimated for the RR Lyrae stars. A detailed search for SX Phe stars in the Blue Straggler region was conducted but none were discovered. If SX Phe exist in the cluster then their amplitudes must be smaller than the detection limit of our photometry. The colour-magnitude diagram has been corrected for heavy differential reddening using the detailed extinction map of the cluster of Alonso-Garcia et al. (2012, Cat. J/AJ/143/70). This has allowed us to set the mean cluster distance from two independent estimates; from the RRab and RRc absolute magnitudes, we find 8.04±0.19 and 7.88±0.30kpc, respectively. Description: V and i time-series photometry for all confirmed variables in NGC 6333. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 107 34 *General data for all of the confirmed variables in NGC 6333 in the FOV of our images. table2.dat 89 14438 V and i light curves
Note on table3.dat: Stars V22-V34 are new discoveries in this work.
See also: J/AJ/89/1707 : Photographic observations of M9 variable stars (Clement+, 1984) J/AJ/112/618 : CCD photometry of variable stars in M9 (Clement+, 1996) J/AJ/101/1352 : Observations of variable stars in M9 (Clement+, 1991) J/AJ/118/453 : M9 RR Lyrae CCD observations (Clement+, 1999) J/AJ/143/70 : Differential reddening in Milky Way globulars (Alonso-Garcia+, 2012) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 3 A3 --- VName Variable name (V1 to V34, V22-V34 are new), <Cl* NGC 6333 SAW VNN> in Simbad 5- 11 A7 --- VType Variable type (1) 12 A1 --- n_VType [c] c: Possibly EA 14- 19 F6.3 mag <Vmag> Average V magnitude 21- 26 F6.3 mag <imag> ?=- Average i magnitude 28 A1 --- l_AV Limit flag on AV 29- 33 F5.3 mag AV Absorption in V band 34 A1 --- n_AV [b] b: Depth of eclipse 36 A1 --- l_Ai Limit flag on Ai 37- 41 F5.3 mag Ai ?=- Absorption in i band 42 A1 --- n_Ai [b] b: Ai lists the depth of eclipse 45- 53 F9.7 d Per ? Period, from this work 54 A1 --- n_Per [d] d: the real period may be twice this value 56- 60 F5.2 d/Myr beta ? Secular period change β=dP/dt 62- 70 F9.4 d HJDmax ?=- Time of maximum eclipse (HJD-2450000) 71 A1 --- n_HJDmax [a] a: Time of minimum light 72- 82 F11.7 d Per1 ?=- Period from Clements papers (2) 85- 86 I2 h RAh Right ascension (J2000) 88- 89 I2 min RAm Right ascension (J2000) 91- 95 F5.2 s RAs Right ascension (J2000) 97 A1 --- DE- Declination sign (J2000) 98- 99 I2 deg DEd Declination (J2000) 101-102 I2 arcmin DEm Declination (J2000) 104-107 F4.1 arcsec DEs Declination (J2000)
Note (1): Labels 'Bl' and 'd' are for Blazhko variables and double-mode RR Lyrae, respectively; 'An.Cep' stands for Anomalous Cepheid, 'E' for Eclising binary (possibly EA), 'EW' for contact eclipsing binaries (W UMa-type), 'LPV' for Long-Period Variable. Note (2): The best previous period estimates for each variable from the Clement series of papers (Clement et al., 1984, Cat. J/AJ/89/1707; Clement & Walker 1991, Cat. J/AJ/101/1352; Clement & Shelton 1996, Cat. J/AJ/112/618, 1999, Cat. J/AJ/118/453) are reported for comparison with our refined periods.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 A3 --- VName Variable name, VNN 5- 9 A5 --- Tel [2.0H 1.5LS] Telescope: 2.0H=2m telescope in Hanle; 1.5LS=1.54m telescope in La Silla, ESO. 11 A1 --- Fltr [VI] Observation filter (V or I) 13- 25 F13.5 d HJD Heliocentric Julian date 27- 32 F6.3 mag magst Standard magnitude 34- 39 F6.3 mag mag Instrumental magnitude 41- 45 F5.3 mag e_mag Error on the magnitude 47- 56 F10.3 s-1 Fref Reference flux (in ADU/s) 58- 63 F6.3 s-1 e_Fref Error on the reference flux (in ADU/s) 65- 74 F10.3 s-1 DFlux Differential flux (in ADU/s) 76- 82 F7.3 s-1 e_DFlux Error on the differential flux (in ADU/s) 84- 89 F6.4 --- p [0.3/1.4] Photometric scale factor
Acknowledgements: Daniel Bramich, dbramich(at) Roberto Figuera, rfiguera(at)
(End) Daniel Bramich [ESO], Patricia Vannier [CDS] 15-Oct-2013
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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