Campaign 9 of the<i>K2</i>Mission: Observational Parameters, Scientific Drivers, and Community Involvement for a Simultaneous Space- and Ground-based Microlensing Survey

Henderson, Calen B.; Poleski, R.; Penny, Matthew T.; Street, R. A.; Bennett, D. P.; Hogg, David W.; Gaudi, B. Scott; Zhu, Wei; Barclay, Thomas; Barentsen, Geert; Howell, Steve B.; Mullally, Fergal; Udalski, A.; Szymański, M. K.; Skowron, J.; Mróz, P.; Kozłowski, S.; Wyrzykowski, Ł.; Pietrukowicz, P.; Ulaczyk, K.; Pawlak, M.; Sumi, T.; Abe, F.; Asakura, Y.; Barry, Richard; Bhattacharya, Atri; Bond, I. A.; Donachie, M.; Freeman, Matthew; Fukui, A.; Hirao, Yuki; Itow, Y.; Koshimoto, Naoki; Li, M. C. A.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Nagakane, M.; Ohnishi, Koji; Oyokawa, H.; Rattenbury, N. J.; Saito, To.; Sharan, A.; Sullivan, D. J.; Tristram, P. J.; Yonehara, A.; Bachelet, E.; Bramich, D. M.; Cassan, A.; Dominik, M.; Jaimes, R. Figuera; Horne, K.; Hundertmark, M.; Mao, Shude; Ranc, Clément; Schmidt, R. W.; Snodgrass, C.; Steele, I. A.; Tsapras, Y.; Wambsganß, J.; Bozza, V.; Burgdorf, M.; Jørgensen, U. G.; Novati, S. Calchi; Ciceri, S.; D’Ago, G.; Evans, D. F.; Hessman, F. V.; Hinse, T. C.; Husser, Tim-Oliver; Mancini, L.; Popovas, A.; Rabus, M.; Rahvar, S.; Scarpetta, G.; Skottfelt, J.; Southworth, J.; Unda-Sanzana, E.; Bryson, S. T.; Caldwell, Douglas A.; Haas, Michael R.; Larson, Kipp A.; McCalmont, Katelynn M.; Packard, M.; Peterson, Colin A.; Putnam, Dustin; Reedy, Lee; Ross, S.; Cleve, Jeffrey E. Van; Akeson, Rachel; Batista, V.; Beaulieu, J. P.; Beichman, Charles; Bryden, G.; Ciardi, David R.; Cole, A. A.; Coutures, C.; Foreman-Mackey, Dan; Fouqué, P.; Friedmann, M.; Gelino, Christopher R.; Kaspi, S.; Kerins, E.; Korhonen, H.; Lang, Dustin; Lee, Chien‐Hsiu; Lineweaver, Charles H.; Maoz, Dan; Marquette, J. B.; Mogavero, Federico; Morales, J. C.; Nataf, David M.; Pogge, Richard W.; Santerne, A.; Shvartzvald, Yossi; Suzuki, D.; Tamura, Motohide; Tisserand, Patrick; Wang, D.

doi:10.1088/1538-3873/128/970/124401

Cited by 88 publications

(43 citation statements)

References 111 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our test result provides an example showing that it is possible to verify the microlens parallax and resolve the degeneracy based on space-based observations, even though the observation is fragmentary. This result gives confidence to other collaborations that will measure the microlens parallax between next-generation microlensing surveys and space telescopes such as the Spitzer microlensing campaign (Yee et al 2015a), K2C9 (Henderson et al 2016), and WFIRST (Spergel et al 2015).…”

Section: Summary and Discussionsupporting

confidence: 57%

OGLE-2016-BLG-0168 Binary Microlensing Event: Prediction and Confirmation of the Microlens Parallax Effect from Space-based Observations

Shin¹,

Udalski²,

Yee³

et al. 2017

Self Cite

View full text Add to dashboard Cite

The microlens parallax is a crucial observable for conclusively identifying the nature of lens systems in microlensing events containing or composed of faint (even dark) astronomical objects such as planets, neutron stars, brown dwarfs, and black holes. With the commencement of a new era of microlensing in collaboration with space-based observations, the microlens parallax can be routinely measured. In addition, space-based observations can provide opportunities to verify the microlens parallax measured from ground-only observations and to find a unique solution to the lensing light-curve analysis. Furthermore, since most space-based observations cannot cover the full light curves of lensing events, it is also necessary to verify the reliability of the information extracted from fragmentary space-based light curves. We conduct a test based on the microlensing event OGLE-2016-BLG-0168, created by a binary lens system consisting of almost equal mass M-dwarf stars, to demonstrate that it is possible to verify the microlens parallax and to resolve degeneracies using the space-based light curve even though the observations are fragmentary. Since space-based observatories will frequently produce fragmentary light curves due to their short observing windows, the methodology of this test will be useful for next-generation microlensing experiments that combine space-based and ground-based collaboration.

show abstract

Section: Summary and Discussionsupporting

confidence: 57%

OGLE-2016-BLG-0168 Binary Microlensing Event: Prediction and Confirmation of the Microlens Parallax Effect from Space-based Observations

Shin¹,

Udalski²,

Yee³

et al. 2017

Self Cite

View full text Add to dashboard Cite

show abstract

“…In addition to these high-cadence, near-continuous survey observations, OGLE-2016-BLG-1190 was observed in two lower-cadence surveys that were specifically motivated to support microlensing in the Kepler microlensing (K2 C9) field (Henderson et al 2016), in which it lies. These surveys, respectively by the 3.6 m Canada-France-Hawaii Telescope (CFHT) and the 3.8 m United Kingdom Infrared Telescope (UKIRT) are both located at the Mauna Kea Observatory in Hawaii.…”

Section: Full Kepler Orbits In Microlensingmentioning

confidence: 97%

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Ryu¹,

Yee²,

Udalski³

et al. 2017

Self Cite

View full text Add to dashboard Cite

We report the discovery of OGLE-2016-BLG-1190Lb, which is likely to be the first Spitzer microlensing planet in the Galactic bulge/bar, an assignation that can be confirmed by two epochs of high-resolution imaging of the combined source-lens baseline object. The planet's mass, M p =13.4±0.9 M J , places it right at the deuteriumburning limit, i.e., the conventional boundary between "planets" and "brown dwarfs." Its existence raises the question of whether such objects are really "planets" (formed within the disks of their hosts) or "failed stars" (lowmass objects formed by gas fragmentation). This question may ultimately be addressed by comparing disk and bulge/bar planets, which is a goal of the Spitzer microlens program. The host is a G dwarf, M host =0.89±0.07 M e , and the planet has a semimajor axis a∼2.0 au. We use Kepler K2 Campaign 9 microlensing data to break the lens-mass degeneracy that generically impacts parallax solutions from Earth-Spitzer observations alone, which is the first successful application of this approach. The microlensing data, derived primarily from near-continuous, ultradense survey observations from OGLE, MOA, and three KMTNet telescopes, contain more orbital information than for any previous microlensing planet, but not quite enough to accurately specify the full orbit. However, these data do permit the first rigorous test of microlensing orbital-motion measurements, which are typically derived from data taken over <1% of an orbital period.

show abstract

“…Therefore, additional techniques (e.g., Pál et al 2016) are required in order to extract the raw light curves of ∼70 K2 C9 late targets (Henderson et al 2016) and 33 microlensing events in the K2 Campaign 11. Nevertheless, our method for interpreting the K2 light curves is applicable to microlensing events both inside and outside the super stamp region.…”

Section: Discussionmentioning

confidence: 99%

“…Indeed, Campaign 9 (C9) of the two-wheeled Kepler mission (K2, Howell et al 2014), or K2 C9, is dedicated for Galactic microlensing observations (Gould & Horne 2013;Henderson et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Extracting Microlensing Signals fromK2Campaign 9

Zhu

Huang

Udalski

et al. 2017

PASP

Self Cite

View full text Add to dashboard Cite

The reduction of the K2 's Campaign 9 (K2 C9) microlensing data is challenging mostly because of the very crowded field and the unstable pointing of the spacecraft. In this work, we present the first method that can extract microlensing signals from this K2 C9 data product. The raw light curves and the astrometric solutions are first derived, using the techniques from Soares-Furtado et al. and Huang et al. for K2 dense field photometry. We then minimize and remove the systematic effect by performing simultaneous modeling with the microlensing signal. We also derive precise (K p − I) vs. (V − I) color-color relations that can predict the microlensing source flux in the Kepler bandpass. By implementing the color-color relation in the light curve modeling, we show that the microlensing parameters can be better constrained. In the end, we use two example microlensing events, OGLE-2016-BLG-0980 and OGLE-2016-BLG-0940, to test our method.

show abstract

Campaign 9 of theK2Mission: Observational Parameters, Scientific Drivers, and Community Involvement for a Simultaneous Space- and Ground-based Microlensing Survey

Cited by 88 publications

References 111 publications

OGLE-2016-BLG-0168 Binary Microlensing Event: Prediction and Confirmation of the Microlens Parallax Effect from Space-based Observations

OGLE-2016-BLG-0168 Binary Microlensing Event: Prediction and Confirmation of the Microlens Parallax Effect from Space-based Observations

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Extracting Microlensing Signals fromK2Campaign 9

Contact Info

Product

Resources

About