Astrophotography by Anthony Ayiomamitis

Differential Photometry - WASP-48 in Cygnus

A variable star, as its name suggests, is a star whose magnitude varies intrinsically, in contrast to eclipsing binaries whose magnitude varies as a result of one star in the binary system eclipsing the other. True variables are one of five types, namely Mira stars, semiregular stars, cepheids, eruptive variables and, finally, cataclysmic variables. Minimum to maximum magnitude can range from days to many months with some variables displaying irregular periods.

A popular method for the study of variable stars, particularly short-term variables, is by the use of the technique known as "differential photometry". Rather than measure the (variable) magnitude of a variable star on an absolute scale, measurements are made over time relative to one or more non-variable star(s) and these differences are then plotted so as to study and illustrate the relative or differential change in magnitude. Due to the very large number of variables stars, the field of differential photometry represents one of the key fields in astronomy whereby the amateur astronomer can make a meaningful and long-lasting contribution to both science and astronomy.

More recently, the search for extrasolar planets (511 discovered so far) has identified yet another interesting application for the practice of differential photometry whereby the minute drops in magnitude of a star hosting an exoplanet are studied. Further details for the interested party are available here.

Note: The light curve for exoplanet WASP-48b in Cygnus depicted below is one of the latest transiting exoplanets, having being announced in Apr/2011, along with WASP-35b and WASP-51b, and represents the fourty-eighth discovery by the WASP (Wide Angle Search for Planets) team. WASP-48b is characterized with a mass 0.98 times that of Jupiter while its radius is equivalent to 1.67 Jupiter radii, thus making this exoplanet one of the larger and least-dense discoveries to-date. WASP-48b requires 191.08 minutes to transit its parent star at a depth of 10.8 mmag or 1.08%. The parent star, GSC 03925-00739, is an evolved star estimated to have a mass of 1.09 solar masses, a radius equivalent to 1.09 solar radii, a temperature of 5,920 K and a visual magnitude of 11.66. Further details regarding WASP-48 and WASP-48b are available in the paper published by the discovery team led by Enoch et al here.

Note: The C- and K-stars used for the purposes of the differential photometry measurements depicted below were GSC 3925:786 (mag 11.3) and GSC 3925:077 (mag 11.3) respectively.

Image Details
Light Curve for Exoplanet WASP-48b
Imaging Details
Parent Star:
WASP-48

GSC/SAO Catalog:
GSC 03925-00739

Constellation:
Cygnus

RA / Dec:
14h 24m 38.97s /
+55 28' 23.8"


Magnitude:
11.66

Distance:
N/A
Exoplanet:
WASP-48b

Period:
2.143634 + 0.000003 d

Transit Duration:
191.08 mins

Transit Depth:
10.8 mmag

Minimum Mass:
0.98 MJup

Radius:
1.67 RJup

Pred Transit Details:
Ingress :  20:07 UT
Mid-trans :  21:42 UT
Egress :  23:18 UT


Date:
July 07-08, 2011
22:45:00 - 03:14:56 UT+3


Location:
Athens, Greece

Equipment:
AP 305/f3.8 Riccardi-Honders
AP 1200GTO GEM
SBIG ST-10XME
SBIG CFW-8A
SBIG LRGB filters


Integrations:
Lum :  219 x 60 sec
Dark :  010 x 60 sec
Flat :  ~22,100 ADU
Binning :  1x1

Temperatures:
Ambient : + 23.0 C
CCD Chip : - 15.0 C

Software:
CCDSoft V5.00.201
AIP4Win V2.2


Processing:
Reduction
Differential Photometry