Research Note
Probing the effect of gravitational microlensing on the measurements of the RossiterMcLaughlin effect
^{1} Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150762 Porto, Portugal
email: moshagh@astro.up.pt
^{2} Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre, 4169007 Porto, Portugal
^{3} Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA
^{4} Institute for Astronomy and NASA Astrobiology Institute, University of HawaiiManoa, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
^{5} Institute for Astronomy and Astrophysics, Department of Computational Physics, University of Tuebingen, 72076 Tuebingen, Germany
Received: 22 July 2013
Accepted: 26 August 2013
In general, in the studies of transit lightcurves and the RossiterMcLaughlin (RM) effect, the contribution of the planet’s gravitational microlensing is neglected. Theoretical studies, have, however shown that the planet’s microlensing can affect the transit lightcurve and in some extreme cases cause the transit depth to vanish. In this paper, we present the results of our quantitative analysis of the contribution of microlensing on the RM effect. Results indicate that for massive planets in longperiod orbits, the planet’s microlensing will have considerable contributions to the star’s RV measurements. We present the details of our study, and discuss our analysis and results.
Key words: planetary systems / techniques: spectroscopic / gravitational lensing: micro / methods: numerical
© ESO, 2013
1. Introduction
In a transiting planetary system, aside from decreasing the flux of the light received from the star, the transiting planet may focus a portion of the light that has been blocked by the planet, through the microlensing effect (Einstein 1936). In general, in studies of transit lightcurves, the contribution of the planet’s gravitational microlensing is neglected. However, it has been shown that in systems with massive or longperiod planets, the microlensing amplification of the stellar flux could be significant, and in the era of high precision photometric observations such as those with the Kepler, it could also be detectable (Sahu & Gilliland 2003; Agol 2003). Using an analytical approach, Sahu & Gilliland (2003) have shown that in some extreme cases, the contribution of the light from the gravitational microlensing may be even so large that the transit lightcurve can vanish. This implies that in order to properly analyze the lightcurve of a transiting system and derive its planetary parameters, the microlensing effect has to also be taken into account (Muirhead et al. 2013).
Fig. 1 Top: schematic configuration of the gravitational microlensing. Bottom: schematic view of the coordinate system used in this study. The origin of the (x,y) coordinate system is at the center of the stellar disk. The quantity r_{p} denotes the planet radius, and r_{∗} is the radius of the star. 

Open with DEXTER 
One important characteristic of a transiting system that can be affected by planet microlensing is the RossiterMcLaughlin effect. As a star rotates around its rotational axis, a given point on its surface will be blueshifted when the star rotates toward the observer and redshifted when it rotates away. During a transit, the corresponding rotational velocity of the portion of the stellar disk that is blocked by the planet is removed from the integration of the velocity over the entire star creating an anomaly in the Radial Velocity (RV) measurements of the star known as the RossiterMcLaughlin (RM) effect (Rossiter 1924; McLaughlin 1924). This effect has been used to constrain the projected rotational velocity of a star (vsini), and the angle between the skyprojections of the stellar spin axis and the planetary orbital plane (λ) (e.g., Hébrard et al. 2008; Winn et al. 2009, 2010; Simpson et al. 2010; Hirano et al. 2011; Albrecht et al. 2012). It is important to note that the determination of vsini and λ can be influenced by second order effects such as the convective blueshift (Shporer & Brown 2011), the differential stellar rotation (Albrecht et al. 2012), and the macroturbulence (Hirano et al. 2011).
Since the physics and geometry behind the RM effect is due to the transiting planet, they are expected to be affected by microlensing in the same way. Probing the significance of the effect of microlensing on the measurements obtained from the RM effect, and quantifying its influence is the main objective of this paper. In Sect. 2, we describe the formalism for the microlensing effect and introduce our theoretical model. In Sect. 3, we show the results of our simulations and discuss the significance of the effect of microlensing and its detectability. In Sect. 4, we conclude our study and present its future applications.
2. Model
We consider a transiting planetary system and assume that the star is an extended source. The surface brightness of the star is considered to follow a quadratic limb darkening law given by (1)In Eq. (1), , and u_{1} and u_{2} are the stellar quadratic limbdarkening coefficients. We consider u_{1} = 0.3 and u_{2} = 0.35, similar to their values for the star HD 209458 in the wavelength range of 582–638 nm (Brown et al. 2001). We also assume that the lens (transiting planet) is an extended object, has zero brightness, and is spherically symmetric. We set the ratio of the planet’s radius to that of the star (r_{p}/r_{∗}) to 0.1, which is similar to the ratio of the radius of Jupiter or a brown dwarf to that of the Sun. The planet is assumed to be on a circular, edgeon orbit. Because the maximum RM effect occurs when the planet orbit is aligned with the stellar rotation axis, we consider the misalignment angle to be zero (λ = 0). We show the distance between the observer and the lens plane by D_{L}, between the observer and the source plane by D_{S}, and between the lens plane and the source plane by D_{LS} (Fig. 1). Using these quantities, the radius of Einstein ring can be written as (Sahu & Gilliland 2003) (2)where M_{L} is the mass of the lens (planet), c is the speed of light, G is the gravitational constant, and we have considered D_{L} ~ D_{S}. As an example, the Einstein ring radius of a Jupitermass planet at 1 AU from a star is ~0.0013 R_{Sun}. For an Earthlike planet at 1 AU, this value becomes ~7.4 × 10^{5} R_{Sun}.
In a system similar to that described above, the distance between a point on the stellar disk and the projection of the center of the lens (planet) on the disk of the star can be written as (3)The lens produces two images of the point (x,y) along the line connecting this point to the center of the projection of the planet on the star’s disk. These images are at distances (4)from the point of the projection of the center of the lens (planet) on the stellar disk, and are visible when they are not occulted by the planet (i.e.,  d_{±}  > r_{p}) (Sahu & Gilliland 2003). We, therefore, define a transmission function T(x,y) as (5)to determine when the effect of the lensedimages have to be taken into account. The amplification caused by these images is given by (Sahu & Gilliland 2003) (6)where δ = d/R_{E}. In order to incorporate the effect of microlensing in the RV measurements (obtained from the RM effect) the profile of the crosscorrelation function (CCF) has to be calculated over the full stellar disk, using the integral (7)In this equation, (8)is the modified stellar surface intensity, and (9)is the velocity profile associated with each point (x,y) due to both the stellar rotation and macroturbulence (Gray 2005). The quantities σ_{∥} and σ_{⊥} in Eq. (9) are given by (10)where ζ is the macroturbulence velocity and is considered to have a value of ζ = 3.98 km s^{1}, equal to that of the Sun (Valenti & Fischer 2005). The quantity σ_{0} is the instrumental broadening which is set to approximately 2.2 km s^{1}. This is equivalent to the broadening of a typical spectrograph with a highresolution of R ~ 110 000 similar to that of HARPS. The velocity v(x,y) in Eq. (9) is defined as (11)where v_{CB} is the convective blueshift and is set to –300 m s^{1}, similar to its value for the Sun (Shporer & Brown 2011).
Fig. 2 Top: graphs of the RM effect with and without the contribution of the planet’s microlensing. Note that the two curves are almost overlaying each other. To remove the effect of microlensing, we assume R_{E} = 0. Bottom: graphs of residuals between the two curves shown in the top panel. The residuals demonstrate the net behavior of microlensing as a function of the planet’s position along the stellar radius. The maximum value of the of microlensing appears at 0.55 stellar radii. 

Open with DEXTER 
3. Calculations and results
We considered a rotating star with vsini = 10 km s^{1} and a planet with a mass of 10 M_{Jup}. We set the value of D_{LS} to 1 AU and let the position of the projection of the planet on the (x,y) plane vary from the outside of the disk of the star (1.2 r_{∗}) to its center.
We used a grid of 4000 × 4000 cells on the (x,y) plane and calculated the integral of Eq. (7). By fitting a Gaussian function to F(v), we determined the center of CCF which corresponds to the value of RV that takes into account the combined contributions from the RM and microlensing effects. To determine the sole effect of microlensing on the value of RM, we carried out similar calculations considering the Einstein ring radius to be zero (R_{E} = 0). By subtracting the results from the results of the previous calculations, we determined the net contribution of the microlensing effect. Figure 2 shows the results. The bottom panel of this figure shows the difference between the results of the two calculations and the contribution of microlensing effect to the RV measurements. As shown here, microlensing has its maximum contribution when the projection of the planet on the stellar disk is at a distance of 0.55 stellar radius from the center of the star. Because we are interested in the maximum effect of microlensing, in the rest of this study, we hold the position of the planet’s projection at (x_{p},y_{p}) = (0.55 r_{∗},0).
To better understand the effects of different parameters on the results, we carried out calculations for different values of the mass and orbital separation of the planet. The mass of the planet was taken to be 0.1, 0.5, 1, 10, and 50 M_{Jup} with its lowest value corresponding to the mass of a Neptunelike object and its largest value being interpreted as the mass of a browndwarf. The orbital separation (D_{LS}) was varied from 0.25 AU to 3 AU in steps of 0.25 AU. We considered the rotational velocity of the host star to be vsini = 2, 5, and 10 km s^{1} (McNally 1965). We also considered three detection limits for RV measurements: 50 cm s^{1} for current facilities such as HARPS, 10 cm s^{1} for observational facilities in the near future such as ESPRESSO at VLT (Pepe et al. 2010), and 2 cm s^{1} for instruments farther in the future such as HIRES at EELT. As shown in Fig. 3, when obtained from all the current and future observational facilities, the microlensing amplification will have significant contribution to the RM measurements of a massive planet in a longperiod orbit (a > 2 AU). For instance, in the case of a 10 Jupitermass planet in a 2 AU orbit around a star with vsini = 10 km s^{1}, the microlensing effect is about 1 m s^{1} which is comparable to the effect of macroturbulence and convective blueshift on RM measurements (~3 − 4 m s^{1}) (Albrecht et al. 2012). In the case of a massive planet on relatively shortperiod orbit (<1 AU), the results depend on the rate of the rotation of the star. If the star is fast rotating, the microlensing effect will be significant, otherwise for slow rotating stars, this effect will be at the detection limit of future facilities such as HIRES at EELT. We note that because the amplitude of the signal associated with the microlensing effect on RM measurements for a planet with a mass of 0.1 M_{Jup} and for all values of its orbital separations are smaller than 0.001 m s^{1}, we excluded these cases from the figure.
Fig. 3 Maximum contribution of microlensing to the measurements of the RM effect for different combination of planet mass and the position of the projection of the planet on the disk of the star. From top to bottom, the stellar rotational velocity is equal to 2, 5, and 10 km s^{1}, respectively. The detection limit of HARPS, ESPRESSO at VLT and HIRES at EELT are also shown for comparison. 

Open with DEXTER 
We also probed the impact of the microlensing on the measured values of the misalignment angle (λ), and the stellar rotation velocity (vsini) obtained from the measurements of the RM effect. Our results indicated that the misalignment angle will not be affected by microlensing. This is an expected result since the measurements of the misalignment angle are sensitive to the asymmetry of the RM signal, and the microlensing effect does not disturb the symmetry of this signal.
We would like to emphasize that in cases where the effect of microlensing is not negligible, both the lightcurve of the star and the RM signal have to be modeled taking this effect into account. In such systems, when fitting the lightcurve, ignoring the microlensing magnification will result in a planetary model in which the radius of the planet is smaller than its actual value. Despite such a discrepancy in the modeled radius of the planet, the vsini obtained from fitting the RM signal is only weakly affected. We note that in systems where the effect of microlensing is included in fitting the lightcurve (Sahu & Gilliland 2003), this effect must also be included in the modeling of the RM signal, otherwise the value of vsini will be underestimated.
4. Analytical analysis
Using the formalism presented by Ohta et al. (2005), we have been able to derive an analytical formula that can roughly reproduce the results of our simulations. As shown by these authors, the averaged value of the radial velocity of the star is given by (12)To use Eq. (12) to determine the variation in the radial velocity (i.e., Δ RV) due to the microlensing effect, we recall that the microlensing effect depends only on the value of the Einstein ring radius R_{E}. This quantity appears in the definition of d_{±} and A_{±}. Taylor expanding these quantities in terms of η = R_{E}/d, one can show that (13)and (14)Equations (13) and (14) indicate that to the second order in R_{E}, A_{−} = 0 and A_{+} = 1, implying that to this order of approximation, the image at d_{−} has no contribution to either the lightcurve or the RM effect. To the lowest order in R_{E}, the microlensing effect simply increases the fraction of the stellar disk that is seen by the observer. In fact, for all points located behind the planet and at distances between r_{p}(1 − η^{2}) and r_{p} from the center of the projection of the planet on the stellar disk, d_{+} > r_{p} implying that to the lowest order, the effect of microlensing is equivalent to reducing the value of the planet radius from r_{p} to . Using Eq. (12), one then obtains (15)The coefficient of proportionality in Eq. (15) can be determined using the results of our numerical experiment. The change in the radial velocity is, therefore, given by (16)
5. Discussion and conclusion
In this study, we explored and quantified the contribution of gravitational microlensing to the measurements of the radial velocity during the transit of a planet (RM effect). We showed that the amplification of the RV signal due to the microlensing effect depends strongly on the mass of the planet and its orbital separation. Results indicated that the effect of microlensing is also significant for massive planets on longperiod orbits, and is detectable with the current observational facilities. Our results showed that microlensing does not disturb the measurements of the misalignment angle caused by the RM effect. If when fitting the lightcurve, this effect is taken into account, it should also be considered in the modeling of the RM signal, otherwise the value of vsini will be underestimated up to several percent for extreme cases. We note that in such cases, the underestimation of the rotational velocity will be within the observational error, and thus undetectable.
Most of the current RM surveys have been carried out on transiting systems that host planets in short period orbits. To better constrain models of planet formation, studies of the RM effect have to also include massive planets in long periods. As those planets orbit mostly fastrotating stars [exoplanets.org], the contribution of microlensing to the measurements of their RM effect will become considerable, and detectable with future observational facilities such as ESPRESSO at VLT and HIRES at EELT.
Acknowledgments
We would like to thank R. Alonso for useful discussions. We acknowledge the support from the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953, and by Fundação para a Ciência e a Tecnologia (FCT) in the form of grants reference SFRH/BD/51981/2012. NCS also acknowledges the support from FCT through program Ciência 2007 funded by FCT/MCTES (Portugal) and POPH/FSE (EC). N.H. acknowledges support from the NAI under Cooperative Agreement NNA09DA77 at the Institute for Astronomy, University of Hawaii, HST grant HSTGO12548.06A, and Alexander von Humboldt Foundation. N.H. is also thankful to the Institute for Astronomy and Astrophysics/Department of Computational Physics at the University of Tuebingen, Germany for their kind hospitality during the course of this project. Support for program HSTGO12548.06A was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS526555.
References
 Agol, E. 2003, ApJ, 594, 449 [NASA ADS] [CrossRef] [Google Scholar]
 Albrecht, S., Winn, J. N., Johnson, J. A., et al. 2012, ApJ, 757, 18 [NASA ADS] [CrossRef] [Google Scholar]
 Brown, T. M., Charbonneau, D., Gilliland, R. L., Noyes, R. W., & Burrows, A. 2001, ApJ, 552, 699 [NASA ADS] [CrossRef] [Google Scholar]
 Einstein, A. 1936, Science, 84, 506 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Gray, D. F. 2005, The Observation and Analysis of Stellar Photospheres (Cambridge: Univeristy Press) [Google Scholar]
 Hébrard, G., Bouchy, F., Pont, F., et al. 2008, A&A, 488, 763 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Hirano, T., Suto, Y., Winn, J. N., et al. 2011, ApJ, 742, 69 [NASA ADS] [CrossRef] [Google Scholar]
 McLaughlin, D. B. 1924, ApJ, 60, 22 [NASA ADS] [CrossRef] [Google Scholar]
 McNally, D. 1965, The Observatory, 85, 166 [NASA ADS] [Google Scholar]
 Muirhead, P. S., Vanderburg, A., Shporer, A., et al. 2013, ApJ, 767, 111 [NASA ADS] [CrossRef] [Google Scholar]
 Ohta, Y., Taruya, A., & Suto, Y. 2005, ApJ, 622, 1118 [NASA ADS] [CrossRef] [Google Scholar]
 Pepe, F. A., Cristiani, S., Rebolo Lopez, R., et al. 2010, in SPIE Conf. Ser., 7735 [Google Scholar]
 Rossiter, R. A. 1924, ApJ, 60, 15 [NASA ADS] [CrossRef] [Google Scholar]
 Sahu, K. C., & Gilliland, R. L. 2003, ApJ, 584, 1042 [NASA ADS] [CrossRef] [Google Scholar]
 Shporer, A., & Brown, T. 2011, ApJ, 733, 30 [NASA ADS] [CrossRef] [Google Scholar]
 Simpson, E. K., Pollacco, D., Hébrard, G., et al. 2010, MNRAS, 405, 1867 [NASA ADS] [Google Scholar]
 Valenti, J. A., & Fischer, D. A. 2005, ApJS, 159, 141 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Winn, J. N., Johnson, J. A., Fabrycky, D., et al. 2009, ApJ, 700, 302 [NASA ADS] [CrossRef] [Google Scholar]
 Winn, J. N., Johnson, J. A., Howard, A. W., et al. 2010, ApJ, 723, L223 [NASA ADS] [CrossRef] [Google Scholar]
All Figures
Fig. 1 Top: schematic configuration of the gravitational microlensing. Bottom: schematic view of the coordinate system used in this study. The origin of the (x,y) coordinate system is at the center of the stellar disk. The quantity r_{p} denotes the planet radius, and r_{∗} is the radius of the star. 

Open with DEXTER  
In the text 
Fig. 2 Top: graphs of the RM effect with and without the contribution of the planet’s microlensing. Note that the two curves are almost overlaying each other. To remove the effect of microlensing, we assume R_{E} = 0. Bottom: graphs of residuals between the two curves shown in the top panel. The residuals demonstrate the net behavior of microlensing as a function of the planet’s position along the stellar radius. The maximum value of the of microlensing appears at 0.55 stellar radii. 

Open with DEXTER  
In the text 
Fig. 3 Maximum contribution of microlensing to the measurements of the RM effect for different combination of planet mass and the position of the projection of the planet on the disk of the star. From top to bottom, the stellar rotational velocity is equal to 2, 5, and 10 km s^{1}, respectively. The detection limit of HARPS, ESPRESSO at VLT and HIRES at EELT are also shown for comparison. 

Open with DEXTER  
In the text 