adsabs/AstroCLIMB huggingface dataset:
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: The phases of the gain solutions recorded for each data set and plotted as a function of frequency for each antenna in both polarizations of the AC tuning (IF). Here, AC refers to a signal pair tuned to the same frequency, where A is the right circular polarization and C is the left circular polarization (https://science.nrao.edu/facilities/vla/docs/manuals/oss/performance/vla-samplers). Each tuning collects 512 MHz of the total bandwidth of 1024 MHz. For all data with no recorded phase values, a value of zero is set as a placeholder.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: Schematic showing an overview of the COSMIC data processing pipeline. There are two data streams: one for real-time system calibration and the other for recording and searching the data for potential technosignatures. The beamformer is designed to create a flexible number of coherent beams, depending on computing resources and workflow. Additionally, the channelization step (Upchannelizer) can be modified to account for different frequency and time resolutions.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: Top: an FPGA server populated with five FPGA cards. Each FPGA board is connected to a pair of quad-port QSFP+ add-on cards, allowing it to interface with a total of 12 QSFP+ modules. This is sufficient to handle the data from two VLA antennas. Bottom: the internal components of a single GPU compute server, comprising six NVIDIA RTX A4000 GPUs, two Highpoint SSD7540 NVMe RAID cards, and two dual-port 100 GbE NICs.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: Back view of the COSMIC DTS rack with each of the components. The image shows the 1 Gb network switch, the primary processing node (head node), and the two 100 GbE switches. The middle panel shows 10 of the 30 demultiplexer units, and the bottom panel shows the back view of the three FPGA servers hosting 15 FPGA cards, into which the 40 and 100 Gb QSFP transceivers are plugged.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: Methanol maser emission from W51M as observed in a coherent beam (red) and an incoherent beam (black). The power ratio is approximately 11% lower than the expected ratio of 23 due to calibration errors. The scatter on the edges arises because the calculation involves taking a ratio of very small numbers.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: Spectra from the W3OH methanol maser source when observed at the boresight (BS; red) and at the half-power point of the primary beam (HPBW; black), both phasing toward the peak position of the maser source as determined from an image generated with data from WIDAR.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: An example of the power spectra within the 2–3 GHz band. The sharp spikes are persistent narrowband RFI, whereas most of the band is free of such features. The “clamshell” shape arises from bandpass filtering using the polyphase filterbank. The channel resolution in these spectra is 8 Hz.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: S/N improvement when adding more antennas.
Paper: COSMIC: An Ethernet-based Commensal, Multimode Digital Backend on the Karl G. Jansky Very Large Array for the Search for Extraterrestrial Intelligence
Authors: C. D. Tremblay, S. S. Varghese, J. Hickish, P. B. Demorest, C. Ng, A. P. V. Siemion, D. Czech, R. A. Donnachie, W. Farah, V. Gajjar, M. Lebofsky, D. H. E. MacMahon, T. Myburgh, M. Ruzindana, J. S. Bright, A. Erickson, K. Lacker
Figure caption: The AlphaData ADM-PCIe-9H7 FPGA card, which supports a powerful AMD XCVU37P FPGA in a PCIe form factor. The platform provides four onboard QSFP+ connections, with the option to add eight more via a pair of AD-PCIE-FQSFP quad-QSFP+ PCIe cards.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption:  RadVel results for HD 112570. Top panel: The best-fit single-planet Keplerian orbital model. The thick black line is the best-fit model, and the colored lines, color-coded by the minimum mass of the planet, indicate the possible orbital solution randomly drawn from MCMC. Middle panel: the residuals to a single Keplerian orbital fit (after subtracting the planet solution). Bottom panel: RVs phase-folded to the ephemeris of the planet. The RV data from HIDES-S, -F1, and -F2 are shown in red circles, triangles, and squares, respectively. The RV data from CES-O and HRS are shown in green and blue circles, respectively.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption: Generalized Lomb–Scargle (GLS) periodograms for HD 112570. (a) GLS periodograms of the observed RVs. (b) Residuals to a single Keplerian orbital fit (after subtracting the planet solution). (c) Window function of sampling. (d) Mean-removed BIS (see Section 5). (e) Hipparcos photometry. The horizontal gray lines, top to bottom, indicate the 0.001, 0.01, and 0.1 false-alarm probability (FAP) levels, respectively. The green shaded area represents the period of the planet signal.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption: HR diagram for two stars. We illustrate the MIST evolutionary track of 1 M ☉, 2 M ☉, and 3 M ☉ stars. The metallicity of 0.0 and −0.5 dex are shown by solid and dashed lines, respectively. Two stars are marked by blue and green open diamonds, respectively. The typical error bar is shown in the bottom left part. Both stars have significantly evolved off the MS phase.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption: Spectra in the region of Ca II H lines. The chromospherically active star HD 120048 is also shown for comparison.
Paper: Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
Authors: Guang-Yao Xiao, Huan-Yu Teng, Jianzhao Zhou, Bun'ei Sato, Yu-Juan Liu, Shaolan Bi, Takuya Takarada, Masayuki Kuzuhara, Marc Hon, Liang Wang, Masashi Omiya, Hiroki Harakawa, Fei Zhao, Gang Zhao, Eiji Kambe, Hideyuki Izumiura, Hiroyasu Ando, Kunio Noguchi, Wei Wang, Meng Zhai, Nan Song, Chengqun Yang, Tanda Li, Timothy D. Brandt, Michitoshi Yoshida, Yoichi Itoh, Eiichiro Kokubo
Figure caption: Fitting results of HD 112570 (left panel) and HD 154391 (right panel). In each panel, the gray line depicts the real data, and the black line shows the data smoothed using a 3μ Hz window. The solid blue line represents the result of MCMC fitting, while the red dashed line corresponds to the fitted Gaussian envelope. Additionally, the green dashed curve corresponds to the three Harvey components, and the brown straight line represents the white noise.
Paper: Statistical Distribution Function of Orbital Spacings in Planetary Systems
Authors: Jeremy Dietrich, Renu Malhotra, Dániel Apai
Figure caption: More results for the Very Closely Packed Set. Top left: scatter plot and histograms of all initial Δ and final Δ for stable systems (in blue) and unstable systems (in orange). Top right: scatter plot and histograms of the planet multiplicity vs. the initial ﹩{{\rm{\Delta }}}_{\min }﹩ distribution stable systems (in blue) and unstable systems (in orange). The green triangles indicate the median of the initial ﹩{{\rm{\Delta }}}_{\min }﹩ for stable systems. Bottom left: the fraction of stable systems vs. planet multiplicity. Bottom right: the fraction of stable systems vs. the mass ratio between the closest nearest-neighbor planet pair.
Paper: Statistical Distribution Function of Orbital Spacings in Planetary Systems
Authors: Jeremy Dietrich, Renu Malhotra, Dániel Apai
Figure caption: More results for the Nominal Kepler Analog Set. Top left: scatter plot and histograms of all initial Δ and final Δ for stable systems (in blue) and unstable systems (in orange). Top right: scatter plot and histograms of the planet multiplicity vs. the initial ﹩{{\rm{\Delta }}}_{\min }﹩ distribution stable systems (in blue) and unstable systems (in orange). The green triangles indicate the median of the initial ﹩{{\rm{\Delta }}}_{\min }﹩ for stable systems. Bottom left: the fraction of stable systems vs. planet multiplicity. Bottom right: the fraction of stable systems vs. the mass ratio between the closest nearest-neighbor planet pair.
Paper: Statistical Distribution Function of Orbital Spacings in Planetary Systems
Authors: Jeremy Dietrich, Renu Malhotra, Dániel Apai
Figure caption: The distribution of initial Δ (nearest-neighbor orbital separations in units of mutual Hill radius) of the Nominal Kepler Analog Set of simulated planetary systems. The random draws we performed generated a roughly log-normal distribution of Δ in a system, as shown by the overplotted fit.
Paper: Statistical Distribution Function of Orbital Spacings in Planetary Systems
Authors: Jeremy Dietrich, Renu Malhotra, Dániel Apai
Figure caption: Results for the Very Closely Packed Set. Top: histogram of all the Δ values for each nearest-neighbor planet pair in stable systems (left) and unstable systems (right). Bottom: histogram of the initial ﹩{{\rm{\Delta }}}_{\min }﹩ distribution and the best-fit log-normal function for stable systems (left) and unstable systems (right).
Paper: Statistical Distribution Function of Orbital Spacings in Planetary Systems
Authors: Jeremy Dietrich, Renu Malhotra, Dániel Apai
Figure caption: Results for the Nominal Kepler Analog Set. Top: histogram of all the Δ values for each nearest-neighbor planet pair in stable systems (left) and unstable systems (right). Bottom: histogram of the initial ﹩{{\rm{\Delta }}}_{\min }﹩ distribution and the best-fit log-normal function for stable systems (left) and unstable systems (right).
Paper: Statistical Distribution Function of Orbital Spacings in Planetary Systems
Authors: Jeremy Dietrich, Renu Malhotra, Dániel Apai
Figure caption: The distribution of initial Δ (nearest-neighbor orbital separations in units of mutual Hill radius) of the Very Closely Packed Set of simulated planetary systems. Note that this distribution is roughly uniform in the range ∼3.5–10 (compare with Figure 1).
Paper: Quasar Microlensing Statistics and Flux-ratio Anomalies in Lens Models
Authors: E. Mediavilla, J. Jiménez-Vicente, V. Motta
Figure caption: Flux-ratio histograms corresponding to single-epoch microlensing obtained using the broad emission lines as reference (thick, black line), peaks in microlensing light curves (thin, blue line), models from Shajib et al. (2019; red shaded histogram), and models from Schmidt et al. (2023; green shaded histogram). Vertical lines show the mean values. The gray-shaded region corresponds to one standard deviation around the mean for single-epoch microlensing and microlensing peaks.
Paper: Quasar Microlensing Statistics and Flux-ratio Anomalies in Lens Models
Authors: E. Mediavilla, J. Jiménez-Vicente, V. Motta
Figure caption: Fractional variations of time delays vs. flux ratios from models obtained for SDSS J2048+1913 changing the exponent of the power-law mass distribution of the lens in the β = 0.5–1.5 range. Each color corresponds to an image pair.
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: Top panel: expected proper motion errors from CASTOR (in blue) as a function of CASTOR g-band magnitude for different total exposure times per epoch, assuming a maximum time baseline of 4 yr. For comparison, typical proper motion uncertainties from Gaia as a function of magnitude are also shown in red, where we converted from the Gaia G band to the CASTOR g band assuming the SED of a turnoff star for an old metal-poor stellar population. Bottom panel: expected plane-of-the-sky velocity precision from CASTOR as a function of the CASTOR g-band magnitude for different distances (solid colored lines), assuming an exposure time of 2200 s per epoch and a maximum time baseline of 4 yr for proper motion measurements. The vertical dotted lines show the approximate magnitude of the main-sequence turnoff at those distances for an old metal-poor stellar population.
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: Synthetic CASTOR UV-u-g-band light curves for a randomly selected flare star (M ⋆ = 0.35 M ⊙, Pleiades member at 112 Myr; Dahm 2015, {m AB,UV = 25.8, m AB,u  = 23.2, m AB,g = 20.0}). The cadence and photometric precision are based on the results from the FORECASTOR ETC for the fiducial observing strategy envisioned for CASTOR’s M star Legacy Survey. Each light curve is offset and normalized by its quiescent flux level. The injected flare was sampled from the GALEX/NUV FFD (Jackman et al. 2023) and is detected at 5.5σ in CASTOR’s UV band. The multiband flare energies are calculated assuming a 9000 K blackbody and likely represent conservative estimates of the u- and g-band flare energies when compared to observations of M star flares with spectroscopic UV instruments such as HST/COS and HST/STIS (e.g., Loyd et al. 2018; Kowalski et al. 2019).
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: Filter response curves for the three baseline CASTOR filters (UV, u, g) and the response functions resulting from a proposed broadband filter that splits the UV and u bands.
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: Evolution of a 0.6 and a 1.2 M ⊙ hydrogen-atmosphere WD in UV–u vs. UV CASTOR magnitude H-R diagram. Points along each cooling track are colored by the age of the WD (as shown in the legend), while the horizontal line denotes the CASTOR limiting magnitude (S/N = 5) in the UV band given a 4200 s exposure. Here, the UV magnitude includes E(B − V) = 0.09 for the LMC.
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: The right side of the GUI, showing plots rendered by the FORECASTOR ETC for synthetic photometry calculations. These photometric calculations and mock aperture renderings update as the user changes and submits different parameters. The panels are resizable and all graphs are interactive (e.g., zoom and pan, show/hide different bands or spectra, obtain the value at a specific position in the graph, download graphs, etc.).
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: The exposure time required to reach S/N = 5 as a function of AB magnitude, assuming a spiral galaxy at z = 1 with R  e  = 0.″25 and n = 1.
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: PSFs for CASTOR's central field of view, in each of its UV (left), u (center), and g bands (right). The original PSF simulations are sampled at 10× CASTOR's pixel scale, and then interpolated to produce a grid that is 20× the telescope’s pixel scale.
Paper: FORECASTOR. I. Finding Optics Requirements and Exposure Times for the Cosmological Advanced Survey Telescope for Optical and UV Research Mission
Authors: Isaac Cheng, Tyrone E. Woods, Patrick Côté, Jennifer Glover, Dhananjhay Bansal, Melissa Amenouche, Madeline A. Marshall, Laurie Amen, John Hutchings, Laura Ferrarese, Kim A. Venn, Michael Balogh, Simon Blouin, Ryan Cloutier, Nolan Dickson, Sarah Gallagher, Martin Hellmich, Vincent Hénault-Brunet, Viraja Khatu, Cameron Lawlor-Forsyth, Cameron Morgan, Harvey Richer, Marcin Sawicki, Robert Sorba
Figure caption: A flowchart describing the workflow associated with CASTOR_ETC’s photometry functionality. The most important parameters and methods of each class are included.