MBCAA Observatory

ASAS1826+12: the eclipsing Cepheid

Observed: 7, 12, 13, 14, 15, 17, 19 July, 5, 18 Aug, 5, 6, 12, 15, 19, 20 Sept, 2, 4, 13, 14, 15, 16, 18 Oct, 3, 8 Nov 2007

Michel Bonnardeau
24 Sept 2007
Revised 27 Sept 2007
Revised 30 Sept 2007 ("weighted" transformation coefficients)
Updated 5 Oct 2007 (more observations)
Revised 10 Oct 2007 (B transformed from TbTbv instead of Tbv, I transformed from R instead of V)
Updated 11 Oct 2007 (one more observation in Rc, transformed from Ic)
Updated 18, 20 Oct, 25 Nov 2007 (more observations)


Multicolor photometric measurements of this Cepheid in an eclipsing binary system (the only known one in our galaxy) are presented.


ASAS1826+12 (actually ASAS182611+1212.6 or ASAS182612 or TYC 1031 01262 1) is the first known Cepheid in an eclipsing binary system in our galaxy (Antipin et al (2007)). The pulsational period is 4.2 days and the orbital period is 51.4 days. Both the primary and secondary eclipses are visible and there is an orbital modulation between them.

The ephemerides are (Antipin et al (2007)):
Pulsation maximum = 2,453,196.529 + 4.1523*E
Primary eclipse minimum = 2,453,571.36 + 51.38*E

The AAVSO issued the Alert Notice 351 (June 8, 2007) to start a campaign of observations of this system (and of KU Her in the same field).


The observations were carried out with a 203mm f/6.3 SC telescope, BVRcIc Johnson-Cousins filters (from Schuler) in a filter wheel and a SBIG ST7E camera (KAF401E CCD). Each exposure is 200s long with one exposure/measurement (no stack).

For the photometry, the comparison star and the check star recommended by the AAVSO are used. They are:

ID RA(J2000) DEC V B-V V-Rc Rc-Ic V-Ic
comp 18:26:09.44 +12:17:37.2 11.914 0.748 0.444 0.432 0.876
check 18:26:23.68 +12:15:47.2 10.892 0.665 0.383 0.358 0.738
(comp is AAVSO chart 070925 star 119).

The phase coverage of the observations:

Red solid line: the orbital phase;
Blue dot line: the pulsational phase;
Red squares: the orbital phases of the V measurements;
Blue circles: the pulsational phases of the V measurements.


The measured b,v magnitudes may be transformed for the instrument response. The transformed B,V magnitudes are then:

V = v + TvTbv*[(b-v)-(Bc-Vc)]
B = b + TbTbv*[(b-v)-(Bc-Vc)]

Bc,Vc are the magnitudes of the comparison star. The transformation coefficients were measured HERE; they are:
TbTbv = 0.002 +/- 0.027
TvTbv = -0.025 +/- 0.015

The transformed R magnitudes (Rc filter) are computed from the observed r magnitudes the same way:

R = r + TrTvr*[(v-r)-(Vc-Rc)]

with the transformation coefficient:
TrTvr = -0.134 +/- 0.017

(one Rc measurement without a match in V in transformed using a Ic measurement).

And the transformed I magnitudes (Ic filter) from the observed i magnitudes:
I = i + TiTri*[(r-i)-(Rc-Ic)]

with the transformation coefficient:
TiTri =0.022 +/- 0.011

Check star

The raw magnitudes and the transformed magnitudes of the check star are:

Blue circles: the raw magnitudes, the error bars are +/- the 1 sigma statistical uncertainties;
Red squares: the transformed magnitudes, the errors bars are computed from the +/- 1 sigma statistical uncertainties on the raw magnitudes and the standard deviations on the transformation coefficients;
11.557 is the magnitude according to the AAVSO.

Pulsational phase analysis

Assuming that the eclipses have a width of 0.25 phase, the transformed magnitudes as a function of the pulsational phases are:

Blue: for the orbital phases around the primary eclipse;
Cyan: for the orbital phases around the secondary eclipse;
Red: all the other (they are still modulated by the orbital movement according to Antipin et al (2007)).
The error bars are computed from the 1 sigma statistical uncertainties on the raw magnitudes and the standard deviations on the transformation coefficients.

Another pulsational phase plot:

The magnitudes are for the orbital phases outside the eclipses:
Blue: B magnitudes;
Green: V magnitudes;
Red: Rc magnitudes;
Brown: Ic magnitudes.

Late by 0.12 pulsational period?

Orbital phase analysis

The diameter of a cepheid is at its maximum when the brightness is diminishing (around phase 0.25) and it is at its minimium when the brightness is on its rise (~0.75); see for example TX Mon.

When the cepheid of this binary system is eclipsed, the eclipse width should then be larger when the diameter is at its maximum.


Antipin S.V., Sokolovsky K.V., Ignatieva T.I. (2007) MNRAS arXiv/astro-ph:0705.0605.

Technical notes

Telescope and camera configuration.

Computer and software configuration.

Transformations for differential photometry.

Transformation coefficients: B, V measurements.

Transformation coefficients: V, Rc measurements.

Transformation coefficients: Rc, Ic measurements.

Astronomical notes

Pulsating stars and its links.

KU Her, a slow irregular variable in the field of view of ASAS1826+12.

Site map


Write to the author

Observations submitted to the AAVSO International Database, observer BZU.
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