The VVV Templates Project 전영범 , 성현일 (KASI)

한장희 , 이종택 ( 한국교원대학교 )

Richard de Grijs (Kavli Institute for Astronomy & Astrophysics)Rodolfo Angeloni (la Pontificia Universidad Catolica(PUC) -Chile)

손정주 ( 한국교원대학교 )

2014 SURVEY SCIENCE GROUP WORKSHOP

VVV Project The Vista Variables in the Vía Láctea (VVV) ESO Public Survey ESO's Visible and Infrared Survey Telescope for Astronomy

4 m telescope a wide near-infrared (IR) camera (VIRCAM) a mosaic of 16 2048x2048 detectors 0.8-2.5 micron an average pixel scale of 0.34"/pixel FoV : 1.1x1.5 square degrees 1 magnitudes deeper than their 2MASS counterparts provide a window into time-variable phenomena a time span of about 5 years, with a total of 1929 hours of observing time

VVV Project Of order 109 point sources within a total sky area of 520 deg2 will

be monitored. The surveyed region includes 36 globular clusters and about 314

known open clusters.  A deep IR atlas in 5 passbands and a catalogue containing

an estimated 106 variable stars.

Light Curve Templates in the Near-IR: Towards Automated Classi-fication of VVV Light Curves for Cataclysmic Variable Stars

Cataclysmic Variables have been extensively observed at optical, ultraviolet, and X-ray wave-lengths, where their white dwarf primary stars and bright accretion disks dominate the spectral en-ergy distribution. Unfortunately, little is known about their infrared properties. The assumption that in-frared observations would reveal only the “uninteresting” secondary star has been shown to be false, as recent investigations have instead shown.

A shorter time-scale it will provide a unique chance of enlarging our specific knowledge of the cata-clysmic phenomenon. In particular, time-series of NIR photometry would allow us to measure the el-lipsoidal variations of the tidally distorted mass-donor star as well as irradiation effects. By modeling the modulation, we could then put strong constraints on fundamental parameters such as the geome-try of the binary, and, in case of the contribution of the mass-donor star in two or more bands is known, it is possible to infer its spectral type (and surface temperature) and to estimate the distance to the binary via photometric parallax.

Light Curve Templates in the Near-IR: Towards Automated Classi-fication of VVV Light Curves for Cataclysmic Variable Stars

Unlike previous variability surveys, such as MACHO and OGLE, the VVV Survey will be carried out in the near-IR, mainly in the K band. While this will allow us to probe deeper into the heavily obscured regions of the Galactic bulge and plane than ever before, it also presents us with important challenges. In particular, the extensive, high-quality templates that are needed for automated variable star classification algorithms are not available in the near-IR. We have thus to build a large database of well-defined, high-quality, near-IR light curves for variable stars of different types, which will form the basis for the VVV automated classification.

This database will be critical for the successful outcome of the VVV Survey.

Light Curve Templates in the Near-IR: Towards Automated Classi-fication of VVV Light Curves for Cataclysmic Variable Stars

In order to properly classify as a template, a light curve must meet some minimum observational criteria

first, the observations must be very precise, with the relative er-ror in the photometry being less than about 1/10 of the light curve amplitude.

Second, the light curve itself must be complete, without any clear gaps. This is of great importance to properly compute accurate Fourier decomposition parameters for the light curves, as needed in order to feed the automated classification algorithms.

Jones et al. (1996)

VVV Templates Project

SCIENTIFIC GOALS The main goal is to derive well-defined light curve templates in

the near-IR for the automated classification of VVV light curves.

RR Lyrae stars in the globular cluster ω Centauri (Del Principe et al. 2006).

VVV Templates Project Targets

# Name α (J2000) δ (J2000) K mag. P[d] Var. type--------------------------------------------------------------------------------------------------01) V Sge 20 20 14.69 +21 06 10.39 9.811 0.5142 Novalike, Supersoft X-ray source02) AE Aqr 20 40 09.16 -00 52 15.07 8.780 0.4151 Intermediate Polar02) UU Aqr 22 09 05.76 -03 46 17.70 12.483 0.1636 SW Sex star03) FO Aqr 22 17 55.38 -08 21 03.90 12.508 0.2018 Intermediate Polar04) AO Psc 22 55 17.99 -03 10 40.00 13.088 0.1496 Intermediate Polar 05) IP Peg 23 23 08.55 +18 24 59.30 11.721 0.1582 Dwarf Novae06) RX And 01 04 35.54 +41 17 57.80 11.56 0.2099 Z Cam star07) HT Cas 01 10 13.13 +60 04 35.40 13.84 0.0736 SU UMa star08) AY Psc 01 36 55.45 +07 16 29.30 14.002 0.0993 Nova-like, RW Tri star09) RW Tri 02 25 36.15 +28 05 50.90 11.46 0.2319 Nova-like variable10) GK Per 03 31 11.82 +43 54 16.80 ~13 1.9968 Intermediate Polar, Fast Novae11) V1309 Ori 05 15 41.41 +01 04 40.50 13.512 0.3326 polar/AM Her system12) U Gem 07 55 05.24 +22 00 05.10 10.83 0.1769 SS Cyg star13) SU UMa 08 12 28.26 +62 36 22.50 11.670 0.0076 Prototype of the SU UMa stars14) Z Cam 08 25 13.20 +73 06 39.23 10.856 0.2898 Prototype of the Z Cam stars15) GY Cnc 09 09 50.55 +18 49 47.50 13.118 0.1754 SS Cyg star

Telescopes

Europe Italy - Osservatorio Astronomico di Padova (INAF-OAPd)

92cm Telescope, delta Scuti, SX Phe

Spain - Instituto de Astrofísica de Canarias (IAC) 1.52m, CAIN III, delta Scuti, SX Phe

Telescopes

Africa IRSF Telescope : 1.4m, RR Lyrae in globular clusters (M62, NGC1851),

delta Scuti in open clusters (NGC6134) 0.75-m Telescope : delta Scuti, SX Phe, Ellipsoidal, Eclipsing binaries

Telescopes

North America Canada Maxico : 2.12 m, CANICA

beta Cephei and delta ScutiSouth America

Chile

Asia Kazakshutan South Korea : 1.8 m BOAO

Bohyunsan Optical Astronomy Observatory (BOAO) 

KASINICS (KASI Near Infrared Camera Sys-tem)

- cooling temperature : sensor part = 30K - temperature of cold box < 80K - Pixel scale : 0.39" x 0.39" - Field of view : 3.3' x 3.3' - Gain(e-/ADU) : 2.56 - Readout Noise : 39 electrons - Dark Current : 18.2 electrons/sec - Average Seeing(BOAO) : 1.5" ~ 1.7" - Filter : total 6 (J, H, Ks, L, H2, H3+)

Light Curve of BL Cam : The Pre l i mi nar y re su l t o f VVV l i ght c u rve t e mpl a te s

R.A. (J2000) 03h 47m 19.8s Dec. (J2000) +63°22’43”

Brightness <V> ~ 13.1mag Period [d/h] 0.03909/0.93834

- Low metallicity ([Fe/H]=-2.4)- High amplitude- Short period and multi - periodicity- One of well known 12 field SX Phe

star

BL Cam, 2MASS

Light Curve of IP Peg : The Pre l i mi nar y re su l t o f VVV l i ght c u rve t e mpl a te s

α(J2000) : 23 23 08.55, δ(J2000) : +18 24 59.30 K mag : 11.721, P[d/h] : 0.1582/3.7968

dwarf nova - U Gem type 동반성에서 백색왜성을 둘러싸고 있는 강착원반으로 물질 유입이 이루어지고 있는 천체 . 불규칙한 주기의 outburst – 가시광에서 2 등급 정도 밝아지는 것으로 알려져 있음 .

Inclination : 80° ～ 85°Mass ratio (q)=0.42Distance = 115±30 pc to the system

Name period(d/h) observation time dataIPPeg 0.1582/3.7968 19:20 – 2:30 8h 관측 (2 주기 )RW Tri 0.2319/5.5656 20:30 – 5:00 7h 관측 (1.3 주기 )UU Aqr 0.1636/3.9264 19:20 – 00:20 5h 관측 (1.2 주 )BL Cam 0.03909/0.93834 20:30 – 5:00 5h 관측 (5 주기 )V1007Cas 0.0332/7.968 19:20 – 4:40 9h 관측 (1.1 주기 )V2416Cyg 0.05589/1.34136 19:20 – 1:00 7h 관측 (5.3 주기 )AY Psc 0.0993/2.3832 20:30 – 4:30KV Per 0.2491/5.9784 19:20 – 5:00 8h 관측 (1.3 주기 )RX And 0.2099/5.0376 19:20 – 5:00 2h 관측 (0.4 주기 )V460And 0.0749808/1.8 20:00 – 5:00 9h 관측 (5 주기 )AM Her 0.1289/3.0936 19:20 – 23:00V1047 Her 0.3207/7.6968 2:30 – 5:00 24h 관측 (3 주기 )BO Lyn 0.0934 / 2.2416 19:20-21:00 36h 관측 (16 주기 )

Light Curve of CVs: The Pre l i mi nar y re su l t o f VVV l i ght c u rve t e mpl a te s

Thank you!