PERIODICITY AND ECLIPSE MINIMA TIMING OF CM DRACONIS
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PERIODICITY AND ECLIPSE MINIMA PERIODICITY AND ECLIPSE MINIMA TIMING OF CM DRACONIS TIMING OF CM DRACONIS CM Draconis (GJ 630.1A, CM Draconis (GJ 630.1A, α α J2000.0 J2000.0 =16h 34m 20.35s, =16h 34m 20.35s, δ δ J2000.0 J2000.0 =+57 =+57 ° ° 09’ 44.7”) is an eclipsing binary 09’ 44.7”) is an eclipsing binary system of magnitude V=12.9 which forms a common proper motion pair with a white dwarf (WD system of magnitude V=12.9 which forms a common proper motion pair with a white dwarf (WD 1633+572) with magnitude V=15 (GJ 630.1B, 1633+572) with magnitude V=15 (GJ 630.1B, α α J2000.0 J2000.0 =16h 34m 21.57s, =16h 34m 21.57s, δ δ J2000.0 J2000.0 =+57 =+57 ° ° 10’ 09.0”) at 10’ 09.0”) at a separation of 26 arcsec. This system has one of the lowest known total mass of 0.44 ∼ a separation of 26 arcsec. This system has one of the lowest known total mass of 0.44 ∼ M M ⊙ ⊙ , at a , at a distance of 14.5pc in the Draco constellation. The system consists of two almost identical M4.5 red distance of 14.5pc in the Draco constellation. The system consists of two almost identical M4.5 red dwarfs orbiting each other with a period of 1.27 days. With its nearly edge-on inclination of ∼ dwarfs orbiting each other with a period of 1.27 days. With its nearly edge-on inclination of ∼ 89.59 89.59 ° ° it was chosen as the target of the first photometric search for planetary transits in the mid it was chosen as the target of the first photometric search for planetary transits in the mid 1990’s. 1990’s. * New linear ephemeris * New linear ephemeris derived derived *Fits against O-C times: *Fits against O-C times: linear, parabolic, linear, parabolic, linear+sinusoidal linear+sinusoidal DATA AND RESULTS DATA AND RESULTS S. Vázquez-Martín S. Vázquez-Martín 1 1 , H. J. Deeg , H. J. Deeg 1,2 1,2 , , S. Dreizler S. Dreizler 3 3 , V. P. Kozhevnikov , V. P. Kozhevnikov 4 4 1. Dpto. de Astrofísica, Universidad de La Laguna, Spain. 1. Dpto. de Astrofísica, Universidad de La Laguna, Spain. 2. Instituto de Astrofísica de Canarias, Spain. 2. Instituto de Astrofísica de Canarias, Spain. 3. Institut für Astrophysik Göttingen, Germany. 3. Institut für Astrophysik Göttingen, Germany. 4. Ural Federal University, Ekaterinburg, Russia. 4. Ural Federal University, Ekaterinburg, Russia. Periodic deviations from a linear ephemeris of a binary star’s eclipses can indicate the presence of a third body in orbit around both Periodic deviations from a linear ephemeris of a binary star’s eclipses can indicate the presence of a third body in orbit around both components. Hints for such a hypothetical companion around the M4.5/M4.5 binary CM Dra were published by Deeg et al. (2000) and components. Hints for such a hypothetical companion around the M4.5/M4.5 binary CM Dra were published by Deeg et al. (2000) and Deeg et al. (2008). The assignment of a planet in the CM Dra system can however only be accepted if the earlier observed periodicity Deeg et al. (2008). The assignment of a planet in the CM Dra system can however only be accepted if the earlier observed periodicity trends can be verified through further observations over several years. For eclipsing binary stars of low mass, the method of eclipse trends can be verified through further observations over several years. For eclipsing binary stars of low mass, the method of eclipse minimum timing allows one to set mass limits for the detection of a third body. Deeg et al. (2008) concluded that the two possibilities minimum timing allows one to set mass limits for the detection of a third body. Deeg et al. (2008) concluded that the two possibilities for the source of CM Dra’s timing variations that remain valid are a planet of a few Jupiter masses on a two decade-long orbit, or an for the source of CM Dra’s timing variations that remain valid are a planet of a few Jupiter masses on a two decade-long orbit, or an object on a century-to-millenium long orbit with masses 1.5M object on a century-to-millenium long orbit with masses 1.5M J J <M <M perturber perturber <0.1M <0.1M ⊙ ⊙ . However, they concluded that it is necessary to do . However, they concluded that it is necessary to do continued observations of the timing of CM Dra’s eclipses to be decisive regarding the continued viability of the sinusoidal-fit-model, continued observations of the timing of CM Dra’s eclipses to be decisive regarding the continued viability of the sinusoidal-fit-model, and hence, about the validity of a Jovian-type planet in a circumbinary orbiting around the CM Dra system. In this work, we update the and hence, about the validity of a Jovian-type planet in a circumbinary orbiting around the CM Dra system. In this work, we update the analysis of Deeg et al. (2008), including further data presented in Morales et al. (2009) and new observations taken at Ural analysis of Deeg et al. (2008), including further data presented in Morales et al. (2009) and new observations taken at Ural Observatory, Russia, during 2008-2013. Eclipse minimum times of all new observations were obtained using the Kwee-van-Woerden Observatory, Russia, during 2008-2013. Eclipse minimum times of all new observations were obtained using the Kwee-van-Woerden method. method. Questions? Find and ask me directly or [email protected] CONCLUSIONS CONCLUSIONS * * MCMC method MCMC method * * χ χ 2 2 (chi-square) (chi-square) * BIC * BIC * Periodogram * Periodogram * Apsidal motion * Apsidal motion ANALYSIS PERFORMED ON O-C ANALYSIS PERFORMED ON O-C DIAGRAM DIAGRAM CM DRACONIS CM DRACONIS ABSTRACT ABSTRACT * * Up (left to right) Up (left to right) : : Linear, parabolic and linear+sinusoidal fits for primary eclipses taking into account Linear, parabolic and linear+sinusoidal fits for primary eclipses taking into account the early data from Lacy (1977) and not taking them into account. the early data from Lacy (1977) and not taking them into account. * * Center (left to right) Center (left to right) : : Histograms of T Histograms of T 0 and P. Scatter diagram of the MCMC parameter values. and P. Scatter diagram of the MCMC parameter values. * * Bottom (left to right) Bottom (left to right) : : The full light curve of CM Dra using the 1.2m Oskar-Lühning-Teleskop (OLT) in The full light curve of CM Dra using the 1.2m Oskar-Lühning-Teleskop (OLT) in Germany. A Lomb-Scargle periodogram from O-C residuals versus the linear ephemeris of the CM Dra Germany. A Lomb-Scargle periodogram from O-C residuals versus the linear ephemeris of the CM Dra system for primary (red) and secondary (blue) eclipses. system for primary (red) and secondary (blue) eclipses. DOWNLOAD DOWNLOAD 420 AUs = 25.7” (d A-B = 3.76R ⊙ ) BIBLIOGRAPHY: Deeg et al. (2000), Deeg et al. (2008), Lacy (1977) and Morales et al. (2009). BIBLIOGRAPHY: Deeg et al. (2000), Deeg et al. (2008), Lacy (1977) and Morales et al. (2009). * Data are best fitted by a parabolic or a * Data are best fitted by a parabolic or a linear+sinusoidal fit. linear+sinusoidal fit. * No indications for non-linear O-C times * No indications for non-linear O-C times when omitting early data from Lacy (1977). when omitting early data from Lacy (1977). * For now, we can not verify the validity of * For now, we can not verify the validity of a Jovian-type planet in a circumbinary orbit a Jovian-type planet in a circumbinary orbit around the CM Dra system, so it will be around the CM Dra system, so it will be necessary to continue with minimum time necessary to continue with minimum time observations of CM Dra’s eclipses. observations of CM Dra’s eclipses. Table 1: Table 1: BIC values of BIC values of primary (first lines) and primary (first lines) and secondary (second lines) secondary (second lines) eclipses of the linear, eclipses of the linear, parabolic and parabolic and linear+sinusoidal fits. linear+sinusoidal fits. Table 2: Table 2: Without the early Without the early data data from Lacy (1977). BIC from Lacy (1977). BIC values of primary (first values of primary (first lines) and secondary lines) and secondary (second lines) eclipses of (second lines) eclipses of the linear, parabolic and the linear, parabolic and linear+sinusoidal fits. linear+sinusoidal fits.
Transcript of PERIODICITY AND ECLIPSE MINIMA TIMING OF CM DRACONIS
PERIODICITY AND ECLIPSE MINIMA PERIODICITY AND ECLIPSE MINIMA TIMING OF CM DRACONISTIMING OF CM DRACONIS
CM Draconis (GJ 630.1A, CM Draconis (GJ 630.1A, ααJ2000.0J2000.0=16h 34m 20.35s, =16h 34m 20.35s, δδJ2000.0J2000.0=+57=+57°° 09’ 44.7”) is an eclipsing binary 09’ 44.7”) is an eclipsing binary system of magnitude V=12.9 which forms a common proper motion pair with a white dwarf (WD system of magnitude V=12.9 which forms a common proper motion pair with a white dwarf (WD 1633+572) with magnitude V=15 (GJ 630.1B, 1633+572) with magnitude V=15 (GJ 630.1B, ααJ2000.0J2000.0=16h 34m 21.57s, =16h 34m 21.57s, δδJ2000.0J2000.0=+57=+57°° 10’ 09.0”) at 10’ 09.0”) at a separation of 26 arcsec. This system has one of the lowest known total mass of 0.44∼a separation of 26 arcsec. This system has one of the lowest known total mass of 0.44∼ MM⊙⊙, at a , at a distance of 14.5pc in the Draco constellation. The system consists of two almost identical M4.5 red distance of 14.5pc in the Draco constellation. The system consists of two almost identical M4.5 red dwarfs orbiting each other with a period of 1.27 days. With its nearly edgeon inclination of ∼dwarfs orbiting each other with a period of 1.27 days. With its nearly edgeon inclination of ∼89.5989.59° ° it was chosen as the target of the first photometric search for planetary transits in the mid it was chosen as the target of the first photometric search for planetary transits in the mid 1990’s. 1990’s.
* New linear ephemeris * New linear ephemeris derived derived *Fits against OC times: *Fits against OC times: linear, parabolic, linear, parabolic, linear+sinusoidallinear+sinusoidal
DATA AND RESULTSDATA AND RESULTS
S. Vázquez-MartínS. Vázquez-Martín11, H. J. Deeg, H. J. Deeg1,21,2, , S. DreizlerS. Dreizler33, V. P. Kozhevnikov, V. P. Kozhevnikov4 4
1. Dpto. de Astrofísica, Universidad de La Laguna, Spain.1. Dpto. de Astrofísica, Universidad de La Laguna, Spain.2. Instituto de Astrofísica de Canarias, Spain.2. Instituto de Astrofísica de Canarias, Spain.3. Institut für Astrophysik Göttingen, Germany.3. Institut für Astrophysik Göttingen, Germany.
4. Ural Federal University, Ekaterinburg, Russia. 4. Ural Federal University, Ekaterinburg, Russia.
Periodic deviations from a linear ephemeris of a binary star’s eclipses can indicate the presence of a third body in orbit around both Periodic deviations from a linear ephemeris of a binary star’s eclipses can indicate the presence of a third body in orbit around both components. Hints for such a hypothetical companion around the M4.5/M4.5 binary CM Dra were published by Deeg et al. (2000) and components. Hints for such a hypothetical companion around the M4.5/M4.5 binary CM Dra were published by Deeg et al. (2000) and Deeg et al. (2008). The assignment of a planet in the CM Dra system can however only be accepted if the earlier observed periodicity Deeg et al. (2008). The assignment of a planet in the CM Dra system can however only be accepted if the earlier observed periodicity trends can be verified through further observations over several years. For eclipsing binary stars of low mass, the method of eclipse trends can be verified through further observations over several years. For eclipsing binary stars of low mass, the method of eclipse minimum timing allows one to set mass limits for the detection of a third body. Deeg et al. (2008) concluded that the two possibilities minimum timing allows one to set mass limits for the detection of a third body. Deeg et al. (2008) concluded that the two possibilities for the source of CM Dra’s timing variations that remain valid are a planet of a few Jupiter masses on a two decadelong orbit, or an for the source of CM Dra’s timing variations that remain valid are a planet of a few Jupiter masses on a two decadelong orbit, or an object on a centurytomillenium long orbit with masses 1.5Mobject on a centurytomillenium long orbit with masses 1.5MJJ<M<Mperturberperturber<0.1M<0.1M⊙⊙. However, they concluded that it is necessary to do . However, they concluded that it is necessary to do continued observations of the timing of CM Dra’s eclipses to be decisive regarding the continued viability of the sinusoidalfitmodel, continued observations of the timing of CM Dra’s eclipses to be decisive regarding the continued viability of the sinusoidalfitmodel, and hence, about the validity of a Joviantype planet in a circumbinary orbiting around the CM Dra system. In this work, we update the and hence, about the validity of a Joviantype planet in a circumbinary orbiting around the CM Dra system. In this work, we update the analysis of Deeg et al. (2008), including further data presented in Morales et al. (2009) and new observations taken at Ural analysis of Deeg et al. (2008), including further data presented in Morales et al. (2009) and new observations taken at Ural Observatory, Russia, during 20082013. Eclipse minimum times of all new observations were obtained using the KweevanWoerden Observatory, Russia, during 20082013. Eclipse minimum times of all new observations were obtained using the KweevanWoerden method. method.
Questions? Find and ask me directly or
CONCLUSIONSCONCLUSIONS
* * MCMC methodMCMC method ** χ χ22 (chisquare) (chisquare) * BIC * BIC * Periodogram * Periodogram * Apsidal motion* Apsidal motion
ANALYSIS PERFORMED ON OC ANALYSIS PERFORMED ON OC DIAGRAMDIAGRAM
CM DRACONISCM DRACONIS
ABSTRACTABSTRACT
* * Up (left to right)Up (left to right):: Linear, parabolic and linear+sinusoidal fits for primary eclipses taking into account Linear, parabolic and linear+sinusoidal fits for primary eclipses taking into account the early data from Lacy (1977) and not taking them into account.the early data from Lacy (1977) and not taking them into account.* * Center (left to right)Center (left to right):: Histograms of T Histograms of T
00 and P. Scatter diagram of the MCMC parameter values. and P. Scatter diagram of the MCMC parameter values.
* * Bottom (left to right)Bottom (left to right):: The full light curve of CM Dra using the 1.2m OskarLühningTeleskop (OLT) in The full light curve of CM Dra using the 1.2m OskarLühningTeleskop (OLT) in Germany. A LombScargle periodogram from OC residuals versus the linear ephemeris of the CM Dra Germany. A LombScargle periodogram from OC residuals versus the linear ephemeris of the CM Dra system for primary (red) and secondary (blue) eclipses.system for primary (red) and secondary (blue) eclipses.
DOWNLOADDOWNLOAD
420 AUs = 25.7”
(dA-B
= 3.76R⊙)
BIBLIOGRAPHY: Deeg et al. (2000), Deeg et al. (2008), Lacy (1977) and Morales et al. (2009). BIBLIOGRAPHY: Deeg et al. (2000), Deeg et al. (2008), Lacy (1977) and Morales et al. (2009).
* Data are best fitted by a parabolic or a * Data are best fitted by a parabolic or a linear+sinusoidal fit.linear+sinusoidal fit.
* No indications for nonlinear OC times * No indications for nonlinear OC times when omitting early data from Lacy (1977).when omitting early data from Lacy (1977).
* For now, we can not verify the validity of * For now, we can not verify the validity of a Joviantype planet in a circumbinary orbit a Joviantype planet in a circumbinary orbit around the CM Dra system, so it will be around the CM Dra system, so it will be necessary to continue with minimum time necessary to continue with minimum time observations of CM Dra’s eclipses.observations of CM Dra’s eclipses.
Table 1:Table 1: BIC values ofBIC values ofprimary (first lines) and primary (first lines) and secondary (second lines) secondary (second lines) eclipses of the linear, eclipses of the linear, parabolic and parabolic and linear+sinusoidal fits.linear+sinusoidal fits.
Table 2:Table 2: Without the early Without the early datadata from Lacy (1977). BIC from Lacy (1977). BIC values of primary (first values of primary (first lines) and secondary lines) and secondary (second lines) eclipses of (second lines) eclipses of the linear, parabolic and the linear, parabolic and linear+sinusoidal fits.linear+sinusoidal fits.
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