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1. Recovering simulated planet and disk signals using SCALES aperture masking

Author

Lach, Mackenzie, Sallum, Steph, Banyal, Ravinder, Batalha, Natalie, Blake, Geoff, Brandt, Tim, Briesemeister, Zackery, Desai, Aditi, Eisner, Josh, Fong, Wen-fai, Greene, Tom, Honda, Mitsuhiko, Kain, Isabel, Kilpatrick, Charlie, de Kleer, Katherine, Liu, Michael, Macintosh, Bruce, Martinez, Raquel, Mawet, Dimitri, Miles, Brittany, Morley, Caroline, de Pater, Imke, Powell, Diana, Sheehan, Patrick, Skemer, Andrew, Spilker, Justin, Stelter, Deno, Stone, Jordan, Surya, Arun, Thirupathi, Sivarani, Wagner, Kevin, Zhou, Yifan, Lach, Mackenzie, Sallum, Steph, Banyal, Ravinder, Batalha, Natalie, Blake, Geoff, Brandt, Tim, Briesemeister, Zackery, Desai, Aditi, Eisner, Josh, Fong, Wen-fai, Greene, Tom, Honda, Mitsuhiko, Kain, Isabel, Kilpatrick, Charlie, de Kleer, Katherine, Liu, Michael, Macintosh, Bruce, Martinez, Raquel, Mawet, Dimitri, Miles, Brittany, Morley, Caroline, de Pater, Imke, Powell, Diana, Sheehan, Patrick, Skemer, Andrew, Spilker, Justin, Stelter, Deno, Stone, Jordan, Surya, Arun, Thirupathi, Sivarani, Wagner, Kevin, and Zhou, Yifan

Abstract

The Slicer Combined with Array of Lenslets for Exoplanet Spectroscopy (SCALES) instrument is a lenslet-based integral field spectrograph that will operate at 2 to 5 microns, imaging and characterizing colder (and thus older) planets than current high-contrast instruments. Its spatial resolution for distant science targets and/or close-in disks and companions could be improved via interferometric techniques such as sparse aperture masking. We introduce a nascent Python package, NRM-artist, that we use to design several SCALES masks to be non-redundant and to have uniform coverage in Fourier space. We generate high-fidelity mock SCALES data using the scalessim package for SCALES' low spectral resolution modes across its 2 to 5 micron bandpass. We include realistic noise from astrophysical and instrument sources, including Keck adaptive optics and Poisson noise. We inject planet and disk signals into the mock datasets and subsequently recover them to test the performance of SCALES sparse aperture masking and to determine the sensitivity of various mask designs to different science signals.

Published
2023
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2. Simulating medium-spectral-resolution exoplanet characterization with SCALES angular/reference differential imaging

Author

Desai, Aditi, Sallum, Stephanie E., Banyal, Ravinder, Batalha, Natalie, Batalha, Natasha, Blake, Geoff, Brandt, Tim, Briesemeister, Zack, de Kleer, Katherine, de Pater, Imke, Eisner, Josh, Fong, Wen-fai, Greene, Tom, Honda, Mitsuhiko, Kain, Isabel, Kilpatrick, Charlie, Lach, Mackenzie, Liu, Mike, Macintosh, Bruce, Martinez, Raquel A., Mawet, Dimitri, Miles, Brittany, Morley, Caroline, Powell, Diana, Sheehan, Patrick, Skemer, Andrew J., Spilker, Justin, Stelter, R. Deno, Stone, Jordan, Surya, Arun, Thirupathi, Sivarani, Wagner, Kevin, Zhou, Yifan, Desai, Aditi, Sallum, Stephanie E., Banyal, Ravinder, Batalha, Natalie, Batalha, Natasha, Blake, Geoff, Brandt, Tim, Briesemeister, Zack, de Kleer, Katherine, de Pater, Imke, Eisner, Josh, Fong, Wen-fai, Greene, Tom, Honda, Mitsuhiko, Kain, Isabel, Kilpatrick, Charlie, Lach, Mackenzie, Liu, Mike, Macintosh, Bruce, Martinez, Raquel A., Mawet, Dimitri, Miles, Brittany, Morley, Caroline, Powell, Diana, Sheehan, Patrick, Skemer, Andrew J., Spilker, Justin, Stelter, R. Deno, Stone, Jordan, Surya, Arun, Thirupathi, Sivarani, Wagner, Kevin, and Zhou, Yifan

Abstract

SCALES (Slicer Combined with Array of Lenslets for Exoplanet Spectroscopy) is a 2 - 5 micron high-contrast lenslet-based integral field spectrograph (IFS) designed to characterize exoplanets and their atmospheres. The SCALES medium-spectral-resolution mode uses a lenslet subarray with a 0.34 x 0.36 arcsecond field of view which allows for exoplanet characterization at increased spectral resolution. We explore the sensitivity limitations of this mode by simulating planet detections in the presence of realistic noise sources. We use the SCALES simulator scalessim to generate high-fidelity mock observations of planets that include speckle noise from their host stars, as well as other atmospheric and instrumental noise effects. We employ both angular and reference differential imaging as methods of disentangling speckle noise from the injected planet signals. These simulations allow us to assess the feasibility of speckle deconvolution for SCALES medium resolution data, and to test whether one approach outperforms another based on planet angular separations and contrasts.

Published
2023

3. The Slicer Combined with Array of Lenslets for Exoplanet Spectroscopy (SCALES): driving science cases and expected outcomes

Author

Sallum, Steph, Skemer, Andrew, Stelter, Deno, Banyal, Ravinder, Batalha, Natalie, Batalha, Natasha, Blake, Geoff, Brandt, Tim, Briesemeister, Zack, de Kleer, Katherine, de Pater, Imke, Desai, Aditi, Eisner, Josh, Fong, Wen-fai, Greene, Tom, Honda, Mitsuhiko, Jensen-Clem, Rebecca, Kain, Isabel, Kilpatrick, Charlie, Kupke, Renate, Lach, Mackenzie, Liu, Michael C., Macintosh, Bruce, Martinez, Raquel A., Mawet, Dimitri, Miles, Brittany, Morley, Caroline, Powell, Diana, Sethuram, Ramya, Sheehan, Patrick, Spilker, Justin, Stone, Jordan, Surya, Arun, Thirupathi, Sivarani, Unni, Athira, Wagner, Kevin, Zhou, Yifan, Sallum, Steph, Skemer, Andrew, Stelter, Deno, Banyal, Ravinder, Batalha, Natalie, Batalha, Natasha, Blake, Geoff, Brandt, Tim, Briesemeister, Zack, de Kleer, Katherine, de Pater, Imke, Desai, Aditi, Eisner, Josh, Fong, Wen-fai, Greene, Tom, Honda, Mitsuhiko, Jensen-Clem, Rebecca, Kain, Isabel, Kilpatrick, Charlie, Kupke, Renate, Lach, Mackenzie, Liu, Michael C., Macintosh, Bruce, Martinez, Raquel A., Mawet, Dimitri, Miles, Brittany, Morley, Caroline, Powell, Diana, Sethuram, Ramya, Sheehan, Patrick, Spilker, Justin, Stone, Jordan, Surya, Arun, Thirupathi, Sivarani, Unni, Athira, Wagner, Kevin, and Zhou, Yifan

Abstract

The Slicer Combined with Array of Lenslets for Exoplanet Spectroscopy (SCALES) is a $2-5~\mu$m, high-contrast integral field spectrograph (IFS) currently being built for Keck Observatory. With both low ($R\lesssim250$) and medium ($R\sim3500-7000$) spectral resolution IFS modes, SCALES will detect and characterize significantly colder exoplanets than those accessible with near-infrared ($\sim1-2~\mu$m) high-contrast spectrographs. This will lead to new progress in exoplanet atmospheric studies, including detailed characterization of benchmark systems that will advance the state of the art of atmospheric modeling. SCALES' unique modes, while designed specifically for direct exoplanet characterization, will enable a broader range of novel (exo)planetary observations as well as galactic and extragalactic studies. Here we present the science cases that drive the design of SCALES. We describe an end-to-end instrument simulator that we use to track requirements, and show simulations of expected science yields for each driving science case. We conclude with a discussion of preparations for early science when the instrument sees first light in $\sim2025$., Comment: 10 pages, 16 figures, submitted to Proceedings of the SPIE

Published
2023

4. Kilonova Spectral Inverse Modelling with Simulation-Based Inference: An Amortized Neural Posterior Estimation Analysis

Author

Darc, P., Bom, Clecio R., Fraga, Bernardo M. O., Kilpatrick, Charlie D., Darc, P., Bom, Clecio R., Fraga, Bernardo M. O., and Kilpatrick, Charlie D.

Abstract

Kilonovae represent a category of astrophysical transients, identifiable as the electromagnetic observable counterparts associated with the coalescence events of binary systems comprising neutron stars and neutron star-black hole pairs. They act as probes for heavy-element nucleosynthesis in astrophysical environments. These studies rely on inference of the physical parameters (e.g., ejecta mass, velocity, composition) that describe kilonovae based on electromagnetic observations. This is a complex inverse problem typically addressed with sampling-based methods such as Markov-chain Monte Carlo (MCMC) or nested sampling algorithms. However, repeated inferences can be computationally expensive due to the sequential nature of these methods. This poses a significant challenge to ensuring the reliability and statistical validity of the posterior approximations and, thus, the inferred kilonova parameters themselves. We present a novel approach: Simulation-Based Inference (SBI) using simulations produced by KilonovaNet. Our method employs an ensemble of Amortized Neural Posterior Estimation (ANPE) with an embedding network to directly predict posterior distributions from simulated spectral energy distributions (SEDs). We take advantage of the quasi-instantaneous inference time of ANPE to demonstrate the reliability of our posterior approximations using diagnostics tools, including coverage diagnostic and posterior predictive checks. We further test our model with real observations from AT2017gfo, the only kilonova with multi-messenger data, demonstrating agreement with previous likelihood-based methods while reducing inference time down to a few seconds. The inference results produced by ANPE appear to be conservative and reliable, paving the way for testable and more efficient kilonova parameter inference.

Published
2023

5. SN 2018agk: A Prototypical Type Ia Supernova with a Smooth Power-law Rise in Kepler (K2)

Author

Wang, Qinan, Rest, Armin, Zenati, Yossef, Ridden-Harper, Ryan, Dimitriadis, Georgios, Narayan, Gautham, Villar, V. Ashley, Magee, Mark R., Foley, Ryan J., Shaya, Edward J., Garnavich, Peter, Wang, Lifan, Hu, Lei, Bodi, Attila, Armstrong, Patrick, Auchettl, Katie, Barclay, Thomas, Barentsen, Geert, Bognár, Zsófia, Brimacombe, Joseph, Bulger, Joanna, Burke, Jamison, Challis, Peter, Chambers, Kenneth, Coulter, David A., Csörnyei, Géza, Cseh, Borbála, Deckers, Maxime, Dotson, Jessie L., Galbany, Lluís, González-Gaitán, Santiago, Gromadzki, Mariusz, Gully-Santiago, Michael, Hanyecz, Ottó, Hedges, Christina, Hiramatsu, Daichi, Hosseinzadeh, Griffin, Howell, D. Andrew, Howell, Steve B., Huber, Mark E., Jha, Saurabh W., Jones, David O., Könyves-Tóth, Réka, Kalup, Csilla, Kilpatrick, Charlie, Kriskovics, Levente, Li, Wenxiong, Lowe, Thomas B, Margheim, Steven, McCully, Curtis, Mitra, Ayan, Muñoz, Jose A., Nicholl, Matt, Nordin, Jakob, Pál, András, Pan, Yen-Chen, Piro, Anthony L, Rest, Sofia, Rino-Silvestre, João, Rojas-Bravo, César, Sárneczky, Krisztián, Siebert, Matthew R., Smartt, Stephen J., Smith, Ken, Sódor, Ádám, Stritzinger, Maximilian D., Szabó, Róbert, Szakáts, Róbert, Tucker, Brad E., Vinkó, József, Wang, Xiaofeng, Wheeler, J. Craig, Young, David R., Zenteno, Alfredo, Zhang, Kaicheng, Zsidi, Gabriella, Wang, Qinan, Rest, Armin, Zenati, Yossef, Ridden-Harper, Ryan, Dimitriadis, Georgios, Narayan, Gautham, Villar, V. Ashley, Magee, Mark R., Foley, Ryan J., Shaya, Edward J., Garnavich, Peter, Wang, Lifan, Hu, Lei, Bodi, Attila, Armstrong, Patrick, Auchettl, Katie, Barclay, Thomas, Barentsen, Geert, Bognár, Zsófia, Brimacombe, Joseph, Bulger, Joanna, Burke, Jamison, Challis, Peter, Chambers, Kenneth, Coulter, David A., Csörnyei, Géza, Cseh, Borbála, Deckers, Maxime, Dotson, Jessie L., Galbany, Lluís, González-Gaitán, Santiago, Gromadzki, Mariusz, Gully-Santiago, Michael, Hanyecz, Ottó, Hedges, Christina, Hiramatsu, Daichi, Hosseinzadeh, Griffin, Howell, D. Andrew, Howell, Steve B., Huber, Mark E., Jha, Saurabh W., Jones, David O., Könyves-Tóth, Réka, Kalup, Csilla, Kilpatrick, Charlie, Kriskovics, Levente, Li, Wenxiong, Lowe, Thomas B, Margheim, Steven, McCully, Curtis, Mitra, Ayan, Muñoz, Jose A., Nicholl, Matt, Nordin, Jakob, Pál, András, Pan, Yen-Chen, Piro, Anthony L, Rest, Sofia, Rino-Silvestre, João, Rojas-Bravo, César, Sárneczky, Krisztián, Siebert, Matthew R., Smartt, Stephen J., Smith, Ken, Sódor, Ádám, Stritzinger, Maximilian D., Szabó, Róbert, Szakáts, Róbert, Tucker, Brad E., Vinkó, József, Wang, Xiaofeng, Wheeler, J. Craig, Young, David R., Zenteno, Alfredo, Zhang, Kaicheng, and Zsidi, Gabriella

Abstract

We present the 30-min cadence Kepler/K2 light curve of the Type Ia supernova (SN Ia) SN 2018agk, covering approximately one week before explosion, the full rise phase and the decline until 40 days after peak. We additionally present ground-based observations in multiple bands within the same time range, including the 1-day cadence DECam observations within the first $\sim$5 days after the first light. The Kepler early light curve is fully consistent with a single power-law rise, without evidence of any bump feature. We compare SN 2018agk with a sample of other SNe~Ia without early excess flux from the literature. We find that SNe Ia without excess flux have slowly-evolving early colors in a narrow range ($g-i\approx -0.20\pm0.20$ mag) within the first $\sim 10$ days. On the other hand, among SNe Ia detected with excess, SN 2017cbv and SN 2018oh tend to be bluer, while iPTF16abc's evolution is similar to normal SNe Ia without excess in $g-i$. We further compare the Kepler light curve of SN 2018agk with companion-interaction models, and rule out the existence of a typical non-degenerate companion undergoing Roche-lobe overflow at viewing angles smaller than $45^{\circ}$., Comment: 20 pages, 14 figures, 5 tables. Published in ApJ

Published
2021
Full Text
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6. SN 2018agk: A Prototypical Type Ia Supernova with a Smooth Power-law Rise in Kepler (K2)

Author

Wang, Qinan, Rest, Armin, Zenati, Yossef, Ridden-Harper, Ryan, Dimitriadis, Georgios, Narayan, Gautham, Villar, V. Ashley, Magee, Mark R., Foley, Ryan J., Shaya, Edward J., Garnavich, Peter, Wang, Lifan, Hu, Lei, Bodi, Attila, Armstrong, Patrick, Auchettl, Katie, Barclay, Thomas, Barentsen, Geert, Bognár, Zsófia, Brimacombe, Joseph, Bulger, Joanna, Burke, Jamison, Challis, Peter, Chambers, Kenneth, Coulter, David A., Csörnyei, Géza, Cseh, Borbála, Deckers, Maxime, Dotson, Jessie L., Galbany, Lluís, González-Gaitán, Santiago, Gromadzki, Mariusz, Gully-Santiago, Michael, Hanyecz, Ottó, Hedges, Christina, Hiramatsu, Daichi, Hosseinzadeh, Griffin, Howell, D. Andrew, Howell, Steve B., Huber, Mark E., Jha, Saurabh W., Jones, David O., Könyves-Tóth, Réka, Kalup, Csilla, Kilpatrick, Charlie, Kriskovics, Levente, Li, Wenxiong, Lowe, Thomas B, Margheim, Steven, McCully, Curtis, Mitra, Ayan, Muñoz, Jose A., Nicholl, Matt, Nordin, Jakob, Pál, András, Pan, Yen-Chen, Piro, Anthony L, Rest, Sofia, Rino-Silvestre, João, Rojas-Bravo, César, Sárneczky, Krisztián, Siebert, Matthew R., Smartt, Stephen J., Smith, Ken, Sódor, Ádám, Stritzinger, Maximilian D., Szabó, Róbert, Szakáts, Róbert, Tucker, Brad E., Vinkó, József, Wang, Xiaofeng, Wheeler, J. Craig, Young, David R., Zenteno, Alfredo, Zhang, Kaicheng, Zsidi, Gabriella, Wang, Qinan, Rest, Armin, Zenati, Yossef, Ridden-Harper, Ryan, Dimitriadis, Georgios, Narayan, Gautham, Villar, V. Ashley, Magee, Mark R., Foley, Ryan J., Shaya, Edward J., Garnavich, Peter, Wang, Lifan, Hu, Lei, Bodi, Attila, Armstrong, Patrick, Auchettl, Katie, Barclay, Thomas, Barentsen, Geert, Bognár, Zsófia, Brimacombe, Joseph, Bulger, Joanna, Burke, Jamison, Challis, Peter, Chambers, Kenneth, Coulter, David A., Csörnyei, Géza, Cseh, Borbála, Deckers, Maxime, Dotson, Jessie L., Galbany, Lluís, González-Gaitán, Santiago, Gromadzki, Mariusz, Gully-Santiago, Michael, Hanyecz, Ottó, Hedges, Christina, Hiramatsu, Daichi, Hosseinzadeh, Griffin, Howell, D. Andrew, Howell, Steve B., Huber, Mark E., Jha, Saurabh W., Jones, David O., Könyves-Tóth, Réka, Kalup, Csilla, Kilpatrick, Charlie, Kriskovics, Levente, Li, Wenxiong, Lowe, Thomas B, Margheim, Steven, McCully, Curtis, Mitra, Ayan, Muñoz, Jose A., Nicholl, Matt, Nordin, Jakob, Pál, András, Pan, Yen-Chen, Piro, Anthony L, Rest, Sofia, Rino-Silvestre, João, Rojas-Bravo, César, Sárneczky, Krisztián, Siebert, Matthew R., Smartt, Stephen J., Smith, Ken, Sódor, Ádám, Stritzinger, Maximilian D., Szabó, Róbert, Szakáts, Róbert, Tucker, Brad E., Vinkó, József, Wang, Xiaofeng, Wheeler, J. Craig, Young, David R., Zenteno, Alfredo, Zhang, Kaicheng, and Zsidi, Gabriella

Abstract

We present the 30-min cadence Kepler/K2 light curve of the Type Ia supernova (SN Ia) SN 2018agk, covering approximately one week before explosion, the full rise phase and the decline until 40 days after peak. We additionally present ground-based observations in multiple bands within the same time range, including the 1-day cadence DECam observations within the first $\sim$5 days after the first light. The Kepler early light curve is fully consistent with a single power-law rise, without evidence of any bump feature. We compare SN 2018agk with a sample of other SNe~Ia without early excess flux from the literature. We find that SNe Ia without excess flux have slowly-evolving early colors in a narrow range ($g-i\approx -0.20\pm0.20$ mag) within the first $\sim 10$ days. On the other hand, among SNe Ia detected with excess, SN 2017cbv and SN 2018oh tend to be bluer, while iPTF16abc's evolution is similar to normal SNe Ia without excess in $g-i$. We further compare the Kepler light curve of SN 2018agk with companion-interaction models, and rule out the existence of a typical non-degenerate companion undergoing Roche-lobe overflow at viewing angles smaller than $45^{\circ}$., Comment: 20 pages, 14 figures, 5 tables. Published in ApJ

Published
2021
Full Text
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