HD 219134 Revisited: Planet d Transit Upper Limit and Planet f Transit Nondetection with ASTERIA and TESS

Seager, Sara; Knapp, Mary; Demory, Brice-Olivier; Krishnamurthy, Akshata; Huang, Chelsea X.; Badenas-Agusti, Mariona; Shporer, Avi; Weisserman, Drew; Becker, Juliette; Vanderburg, Andrew; Smith, Matthew W.; Pong, Christopher M.; Bailey, Vanessa P.; Donner, Amanda; Pasquale, Peter Di; Campuzano, Brian; Smith, Colin H.; Luu, Jason; Babuscia, Alessandra; Bocchino, Robert L.; Loveland, Jessica; Colley, Cody; Gedenk, Tobias; Kulkarni, Tejas; Hughes, Kyle; White, Mary L.; Krajewski, Joel; Fesq, Lorraine; Ricker, G.; Vanderspek, R.; Latham, David W.; Jenkins, Jon M.; Winn, Joshua N.; Caldwell, Douglas A.; Collins, Karen A.; Dragomir, Diana; Fausnaugh, Michael; Glidden, Ana; Schlieder, Joshua E.; Twicken, Joseph D.; Wohler, Bill

doi:10.3847/1538-3881/abcd3d

Cited by 4 publications

(2 citation statements)

References 43 publications

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“…In this section, we present a summary of the α Cen data reduction and photometry, with details of the pipeline described in Knapp et al (2020) and Seager et al (2021).…”

Section: Methodsmentioning

confidence: 99%

“…Although bias frames are typically used to correct for offsets, flat frames are used to correct column-dependent pixel-to-pixel gain variations caused due to the presence of an amplifier and ADC converter at every column and an amplifier at every pixel. We attempted to take on-orbit flat frames by illuminating the detector with scattered sunlight, following the procedure outlined in Knapp et al (2020) and Seager et al (2021). However, these observations failed because the camera did not initialize properly.…”

Section: Cmos Detector and Systematics Calibrationmentioning

confidence: 99%

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Transit Search for Exoplanets around Alpha Centauri A and B with ASTERIA

Krishnamurthy

Knapp

Günther

et al. 2021

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Alpha Centauri is a triple star system with two Sun-like stars, α Cen A (V = 0.01) and B (V = 1.33), and a third fainter red dwarf star, Proxima Centauri. Most current transit missions cannot produce precision photometry of α Cen A and B as their detectors saturate for these very bright stars. The Arcsecond Space Telescope Enabling Research in Astrophysics (ASTERIA) was a technology demonstration mission that successfully demonstrated two key technologies necessary for precision photometry achieving line-of-sight fine-pointing stability of 0.5″ rms and focal plane temperature control of ±0.01 K over a period of 20 minutes. The payload consisted of a 6.7 cm aperture diameter refractive camera and used a scientific complementary metal-oxide semiconductor detector that enabled monitoring of the brightest stars without saturating. We obtained spatially unresolved (blended) observations of α Cen A and B during opportunistic science campaigns as part of ASTERIA's extended mission. The resulting 1σ photometric precision for the blended α Cen A and B data is 250 ppm (parts per million) per 9 s exposure. We do not find evidence of transits in the blended data. We establish limits for transiting exoplanets around both α Cen A and B using transit signal injection and recovery tests. We find that ASTERIA is sensitive to planets with radii as small as 3.0 R ⊕ around α Cen A and 3.7 R ⊕ around α Cen B, corresponding to signals of ∼500 ppm (signal-tonoise ratio = 5.0) in the blended data, with periods ranging from 0.5 to 6 days.

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“…In this section, we present a summary of the α Cen data reduction and photometry, with details of the pipeline described in Knapp et al (2020) and Seager et al (2021).…”

Section: Methodsmentioning

confidence: 99%

Section: Cmos Detector and Systematics Calibrationmentioning

confidence: 99%

Transit Search for Exoplanets around Alpha Centauri A and B with ASTERIA

Krishnamurthy

Knapp

Günther

et al. 2021

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Framework for the architecture of exoplanetary systems

Mishra

Alibert

Udry

et al. 2023

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We present a novel, model-independent framework for studying the architecture of an exoplanetary system at the system level. This framework allows us to characterise, quantify, and classify the architecture of an individual planetary system. Our aim in this endeavour is to generate a systematic method to study the arrangement and distribution of various planetary quantities within a single planetary system. We propose that the space of planetary system architectures be partitioned into four classes: similar, mixed, anti-ordered, and ordered. We applied our framework to observed and synthetic multi-planetary systems, thereby studying their architectures of mass, radius, density, core mass, and the core water mass fraction. We explored the relationships between a system’s (mass) architecture and other properties. Our work suggests that: (a) similar architectures are the most common outcome of planet formation; (b) internal structure and composition of planets shows a strong link with their system architecture; (c) most systems inherit their mass architecture from their core mass architecture; (d) most planets that started inside the ice line and formed in-situ are found in systems with a similar architecture; and (e) most anti-ordered systems are expected to be rich in wet planets, while most observed mass ordered systems are expected to have many dry planets. We find, in good agreement with theory, that observations are generally biased towards the discovery of systems whose density architectures are similar, mixed, or anti-ordered. This study probes novel questions and new parameter spaces for understanding theory and observations. Future studies may utilise our framework to not only constrain the knowledge of individual planets, but also the multi-faceted architecture of an entire planetary system. We also speculate on the role of system architectures in hosting habitable worlds.

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Assessing Exoplanetary System Architectures with DYNAMITE Including Observational Upper Limits

Dietrich

2024

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The information gathered from observing planetary systems is not limited to the discovery of planets, but also includes the observational upper limits constraining the presence of any additional planets. Incorporating these upper limits into statistical analyses of individual systems can significantly improve our ability to find hidden planets in these systems by narrowing the parameter space in which to search. Here, I include radial velocity (RV), transit, and transit timing variation (TTV) upper limits on additional planets in known multiplanet systems into the Dynamite software package and test their impact on the predicted planets for these systems. The tests are run on systems with previous Dynamite analysis and with updated known planet parameters in the 2–3 yr since the original predictions. I find that the RV limits provide the strongest constraints on additional planets, lowering the likelihood of finding them within orbital periods of ∼10–100 days in the inner planetary systems, as well as truncating the likely planet size (radius and/or mass) distributions toward planets smaller than those currently observed. Transit and TTV limits also provide information on the size and inclination distributions of both the known and predicted planets in the system. Utilizing these limits on a wider range of systems in the near future will help determine which systems might be able to host temperate terrestrial planets and contribute to the search for extraterrestrial biosignatures.

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HD 219134 Revisited: Planet d Transit Upper Limit and Planet f Transit Nondetection with ASTERIA and TESS

Cited by 4 publications

References 43 publications

Transit Search for Exoplanets around Alpha Centauri A and B with ASTERIA

Transit Search for Exoplanets around Alpha Centauri A and B with ASTERIA

Framework for the architecture of exoplanetary systems

Assessing Exoplanetary System Architectures with DYNAMITE Including Observational Upper Limits

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