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11 results on '"Calchi Novati, Sebastiano"'

1. OGLE-2015-BLG-0845L: a low-mass M dwarf from the microlensing parallax and xallarap effects.

Author

(胡哲程), Zhecheng Hu, (祝伟), Wei Zhu, Gould, Andrew, Udalski, Andrzej, Sumi, Takahiro, (陈平), Ping Chen, Calchi Novati, Sebastiano, Yee, Jennifer C, Beichman, Charles A, Bryden, Geoffery, Carey, Sean, Fausnaugh, Michael, Gaudi, B Scott, Henderson, Calen B, Shvartzvald, Yossi, Wibking, Benjamin, Mróz, Przemek, Skowron, Jan, Poleski, Radosław, and Szymański, Michał K

Subjects
GRAVITATIONAL lenses, PARALLAX, MASS measurement, MICROLENSES, DATA analysis
Abstract

We present the analysis of the microlensing event OGLE-2015-BLG-0845, which was affected by both the microlensing parallax and xallarap effects. The former was detected via the simultaneous observations from the ground and Spitzer , and the latter was caused by the orbital motion of the source star in a relatively close binary. The combination of these two effects led to a mass measurement of the lens object, revealing a low-mass (⁠|$0.14 \pm 0.05 \, \mathrm{ M}_{\odot }$|⁠) M dwarf at the bulge distance (⁠|$7.6 \pm 1.0$| kpc). The source binary consists of a late F-type subgiant and a K-type dwarf of |$\sim 1.2$| and |$\sim 0.9 \mathrm{ M}_{\odot }$|⁠ , respectively, and the orbital period is |$70 \pm 10$| d. OGLE-2015-BLG-0845 is the first single-lens event in which the lens mass is measured via the binarity of the source. Given the abundance of binary systems as potential microlensing sources, the xallarap effect may not be a rare phenomenon. Our work thus highlights the application of the xallarap effect in the mass determination of microlenses, and the same method can be used to identify isolated dark lenses. [ABSTRACT FROM AUTHOR]

Published
2024
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3. Community Involvement in the WFIRST Exoplanet Microlensing Survey

Author

Bennett, David P., Akeson, Rachel, Barclay, Thomas, Beaulieu, Jean-Phillipe, Bhattacharya, Aparna, Boyd, Padi, Bozza, Valerio, Bryden, Geoffrey, Calchi Novati, Sebastiano, Colon, Knicole, Gaudi, B. Scott, Henderson, Calen B., Hirao, Yuki, Jacklin, Savannah, Koshimoto, Naoki, Lu, Jessica, Penny, Matthew, Poleski, Radek, Quintana, Elisa, Ranc, Clement, Sahu, Kailash C., Street, Rachel, Sumi, Takahiro, Suzuki, Daisuke, Yee, Jennifer, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics
Abstract

WFIRST is NASA's first flagship mission with pre-defined core science programs to study dark energy and perform a statistical census of wide orbit exoplanets with a gravitational microlensing survey. Together, these programs are expected to use more than half of the prime mission observing time. Previously, only smaller, PI-led missions have had core programs that used such a large fraction of the observing time, and in many cases, the data from these PI-led missions was reserved for the PI's science team for a proprietary period that allowed the PI's team to make most of the major discoveries from the data. Such a procedure is not appropriate for a flagship mission, which should provide science opportunities to the entire astronomy community. For this reason, there will be no proprietary period for WFIRST data, but we argue that a larger effort to make WFIRST science accessible to the astronomy community is needed. We propose a plan to enhance community involvement in the WFIRST exoplanet microlensing survey in two different ways. First, we propose a set of high level data products that will enable astronomers without detailed microlensing expertise access to the statistical implications of the WFIRST exoplanet microlensing survey data. And second, we propose the formation of a WFIRST Exoplanet Microlensing Community Science Team that will open up participation in the development of the WFIRST exoplanet microlensing survey to the general astronomy community in collaboration for the NASA selected science team, which will have the responsibility to provide most of the high level data products. This community science team will be open to volunteers, but members should also have the opportunity to apply for funding., Astro2020 APC White Paper

Published
2019

4. Community Involvement in the WFIRST Exoplanet Microlensing Survey

Author

Bennett, David, Akeson, Rachel, Barclay, Thomas, Beaulieu, Jean-Phillipe, Bhattacharya, Aparna, Boyd, Padi, Bozza, Valerio, Bryden, Geoffrey, Calchi Novati, Sebastiano, Colon, Knicole, Gaudi, B. Scott, Henderson, Calen B., Hirao, Yuki, Jacklin, Savannah, Koshimoto, Naoki, Lu, Jessica, Penny, Matthew, Poleski, Radek, Quintana, Elisa, Ranc, Clément, Sahu, Kailash C., Street, Rachel, Sumi, Takahiro, Suzuki, Daisuke, Yee, Jennifer, Aston Business School, Aston University [Birmingham], NASA Ames Research Center Cooperative for Research in Earth Science in Technology (ARC-CREST), NASA Ames Research Center (ARC), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [Berkeley], University of California [Berkeley], University of California-University of California, and goddard space

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

WFIRST is NASA's first flagship mission with predefined core core science programs. We present a set of high level data products that will enable broad participation in the science of the exoplanet microlensing survey and a community science team concept that will allow broad community involvement in the survey development and scientific output.

Published
2019

5. Qatar-2: A K Dwarf Orbited by a Transiting Hot Jupiter and a more Massive Companion in an Outer Orbit

Author

Bryan, Marta L., Fulton, Benjamin J., and Calchi Novati, Sebastiano

Abstract

We report the discovery and initial characterization of Qatar-2b, a hot Jupiter transiting a V = 13.3 mag K dwarf in a circular orbit with a short period, P_b = 1.34 days. The mass and radius of Qatar-2b are M_P = 2.49 M_J and R_P = 1.14 R_J, respectively. Radial-velocity monitoring of Qatar-2 over a span of 153 days revealed the presence of a second companion in an outer orbit. The Systemic Console yielded plausible orbits for the outer companion, with periods on the order of a year and a companion mass of at least several M_J. Thus, Qatar-2 joins the short but growing list of systems with a transiting hot Jupiter and an outer companion with a much longer period. This system architecture is in sharp contrast to that found by Kepler for multi-transiting systems, which are dominated by objects smaller than Neptune, usually with tightly spaced orbits that must be nearly coplanar.

Published
2012

6. High-precision photometry by telescope defocusing – IV. Confirmation of the huge radius of WASP-17 b†

Author

John, Southworth, Dominik, M., Fang, X. S., Harpsoe, K., Jorgensen, U. G., Kerins, E., Liebig, C., Mancini, Luigi, Skottfelt, J., Smalley, D. R. Anderson B., Tregloan Reed, J., Wertz, O., Alsubai, K. A., Bozza, Valerio, CALCHI NOVATI, Sebastiano, Dreizler, S., S. H., Gu, Hinse, T. C., Hundertmark, M., Jessen Hansen, J., Kains, N., Kjeldsen, H., Lund, M. N., Lundkvist, M., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, Gaetano, Snodgrass, C., and Surdej, J.

Subjects
stars: individual: WASP-17, stars: fundamental parameters, stars: individual: WASP-17, stars: fundamental parameters
Published
2012

7. OGLE-2008-BLG-510: first automated real-time detection of a weak microlensing anomaly - brown dwarf or stellar binary?

Author

Bozza, Valerio, Dominik, M., Rattenbury, N. J., Joergensen, U. G., Tsapras, Y., Bramich, D. M., Udalski, A., Bond, I. A., Liebig, C., Fouque, A. Cassan P., Fukui, A., Hundertmark, M., Shin, I. G., Lee, S. H., Choi, J. Y., Park, S. Y., Gould, A., Allan, A., Mao, S., Wyrzykowski, L., Street, R. A., Buckley, D., Nagayama, T., Mathiasen, M., Hinse, T. C., CALCHI NOVATI, Sebastiano, Harpsoee, K., Mancini, Luigi, Scarpetta, Gaetano, Anguita, T., Burgdorf, M. J., Horne, K., Hornstrup, A., Kains, N., Kerins, E., Kjaergaard, P., Masi, G., Rahvar, S., Ricci, D., Snodgrass, C., Southworth, J., Steele, I. A., Surdej, J., Thoene, C. C., Wambsganss, J., Zub, M., Albrow, M. D., Batista, V., Beaulieu, J. P., Bennett, D. P., Caldwell, J. A. R., Cole, A., Cook, K. H., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. B., Martin, R., Menzies, J., Pollard, K. R., Sahu, K. C., Williams, A., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Ulaczyk, K., Depoy, D. L., Dong, S., Han, C., Janczak, J., Lee, C. U., Pogge, R. W., Abe, F., Furusawa, K., Hearnshaw, J. B., Itow, Y., Kilmartin, P. M., Korpela, A. V., Lin, W., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Perrott, Y. C., Saito, T. o., Skuljan, L., Sullivan, D. J., Sumi, T., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Gulbis, A., Hashimoto, Y., Kniazev, A., and Vaisanen, P.

Subjects
gravitational lensing: micro, planetary systems
Published
2012

9. OGLE-2009-BLG-092/MOA-2009-BLG-137: A Dramatic Repeating Event with the Second Perturbation Predicted by Real-time Analysis

Author

Ryu, Y. H., Han, C., Hwang, K. H., Street, R., Udalski, A., Sumi, T., Fukui, A., Beaulieu, J. P., Gould, A., Dominik, M., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Furusawa, K., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Korpela, A., Lin, W., Ling, C. H., Makita, S., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nishimoto, K., Ohnishi, K., Perrott, Y. C., Rattenbury, N., Saito, T. o., Skuljan, L., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Szymański, M. K., Kubiak, M., Pietrzyński, G., Poleski, R., Soszyński, I., Szewczyk, O., Wyrzykowski, Ł., Ulaczyk, K., Bos, M., Christie, G. W., Depoy, D. L., Gal Yam, A., Gaudi, B. S., Kaspi, S., Lee, C. U., Maoz, D., Mccormick, J., Monard, B., Moorhouse, D., Pogge, R. W., Polishook, D., Shvartzvald, Y., Shporer, A., Thornley, G., Yee, J. C., Albrow, M. D., Batista, V., Brillant, S., Cassan, A., Cole, A., Corrales, E., Coutures, C. h., Dieters, S., Fouque, P., Greenhill, J., Menzies, J., Allan, A., Bramich, D. M., Browne, P., Horne, K., Kains, N., Snodgrass46, C., Steele, I., Tsapras, Y., Bozza, Valerio, Burgdorf, M. J., CALCHI NOVATI, Sebastiano, Dreizler, S., Finet, F., Glitrup, M., Grundahl, F., Harpsøe, K., Hessman, F. V., Hinse, T. C., Hundertmark, M., Jørgensen, U. G., Liebig, C., Maier, G., Mancini, Luigi, Mathiasen, M., Rahvar, S., Ricci, D., Scarpetta, Gaetano, Skottfelt, J., Surdej, J., Southworth, J., Wambsganss, J., and Zimmer, F.

Subjects
Physics, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Binary number, Perturbation (astronomy), Astronomy and Astrophysics, Astrophysics, Light curve, Gravitational microlensing, 01 natural sciences, Stars, Settore FIS/05 - Astronomia e Astrofisica, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Bulge, 0103 physical sciences, Orbital motion, Real time analysis, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences
Abstract

We report the result of the analysis of a dramatic repeating gravitational microlensing event OGLE-2009-BLG-092/MOA-2009-BLG-137, for which the light curve is characterized by two distinct peaks with perturbations near both peaks. We find that the event is produced by the passage of the source trajectory over the central perturbation regions associated with the individual components of a wide-separation binary. The event is special in the sense that the second perturbation, occurring $\sim 100$ days after the first, was predicted by the real-time analysis conducted after the first peak, demonstrating that real-time modeling can be routinely done for binary and planetary events. With the data obtained from follow-up observations covering the second peak, we are able to uniquely determine the physical parameters of the lens system. We find that the event occurred on a bulge clump giant and it was produced by a binary lens composed of a K and M-type main-sequence stars. The estimated masses of the binary components are $M_1=0.69 \pm 0.11\ M_\odot$ and $M_2=0.36\pm 0.06\ M_\odot$, respectively, and they are separated in projection by $r_\perp=10.9\pm 1.3\ {\rm AU}$. The measured distance to the lens is $D_{\rm L}=5.6 \pm 0.7\ {\rm kpc}$. We also detect the orbital motion of the lens system., 18 pages, 5 figures, 1 table

Published
2010

10. MICROLENSING EVENTS TOWARDS LMC AND M31.

Author

JETZER, PHILIPPE and CALCHI^NOVATI, SEBASTIANO

Subjects
LARGE magellanic cloud, MICROLENSING (Astrophysics), GRAVITATIONAL lenses, OPTICAL depth (Astrophysics), ANDROMEDA Galaxy, MILKY Way
Published
2005

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