adsabs/AstroCLIMB huggingface dataset:
Paper: Closeby Habitable Exoplanet Survey (CHES). II. An Observation Strategy for the Target Stars
Authors: Dongjie Tan, Jianghui Ji, Chunhui Bao, Xiumin Huang, Guo Chen, Su Wang, Yao Dong, Haitao Li, Junbo Zhang, Liang Fang, Dong Li, Lei Deng, Jiacheng Liu, Zi Zhu
Figure caption: The relative positions of V* AK Lep and * gam Lep on the celestial sphere. While these two stars do not form a binary star system, their close proximity on the celestial sphere allows for simultaneous observation of both targets. The FOV is 0.°44 × 0.°44. Panel (a): image from Aladin Sky Atlas (F. Bonnarel et al. 2000). Panel (b): simulated observational images of the target stars (J. Ji et al. 2023).
Paper: Closeby Habitable Exoplanet Survey (CHES). II. An Observation Strategy for the Target Stars
Authors: Dongjie Tan, Jianghui Ji, Chunhui Bao, Xiumin Huang, Guo Chen, Su Wang, Yao Dong, Haitao Li, Junbo Zhang, Liang Fang, Dong Li, Lei Deng, Jiacheng Liu, Zi Zhu
Figure caption: Observed ranges under different years at each moment. In the first, third, and fifth years, conventional mode type 1 will be used. In the second and fourth years, conventional mode type 2 will be used. To avoid the effects of sunlight, no observations will be conducted in regions 9–12.
Paper: Closeby Habitable Exoplanet Survey (CHES). II. An Observation Strategy for the Target Stars
Authors: Dongjie Tan, Jianghui Ji, Chunhui Bao, Xiumin Huang, Guo Chen, Su Wang, Yao Dong, Haitao Li, Junbo Zhang, Liang Fang, Dong Li, Lei Deng, Jiacheng Liu, Zi Zhu
Figure caption: Distribution of targets in ecliptic coordinates. The distribution is not homogeneous, leading to the need to use the reobservation mode to make adjustments in the observation time.
Paper: Closeby Habitable Exoplanet Survey (CHES). II. An Observation Strategy for the Target Stars
Authors: Dongjie Tan, Jianghui Ji, Chunhui Bao, Xiumin Huang, Guo Chen, Su Wang, Yao Dong, Haitao Li, Junbo Zhang, Liang Fang, Dong Li, Lei Deng, Jiacheng Liu, Zi Zhu
Figure caption: Two types of observation modes (J.-H. Ji et al. 2022). Upper panel: conventional mode. Lower panel: revisited mode.
Paper: Closeby Habitable Exoplanet Survey (CHES). II. An Observation Strategy for the Target Stars
Authors: Dongjie Tan, Jianghui Ji, Chunhui Bao, Xiumin Huang, Guo Chen, Su Wang, Yao Dong, Haitao Li, Junbo Zhang, Liang Fang, Dong Li, Lei Deng, Jiacheng Liu, Zi Zhu
Figure caption: The distribution of the proposed number of observations for each target star is determined by various parameters. The average number of observations was approximately 100. The minimum required number of observations is set at 30, while the maximum number of observations reaches 308.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: Top: the 120 s TESS SAP fluxes for the TOI-1450 system for sectors 14–60. Each sector’s data is mean-normalized. Middle: GLS periodogram of the TESS 120 s data. Dashed vertical lines are drawn on the periodogram corresponding with the peaks at 40 days, 27 days (the length of a single TESS sector), and 2 days. Bottom: TESS photometry of sectors 57–60 the TOI-1450 system. The different sectors are colored differently in order to draw attention to where potential breaks in the baseline are expected. Sinusoidal variations on 40 days and 2 days timescales are obvious in these sectors.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: SED fit (upper black curve) to the observed photometry of TOI-1450A (red symbols). The absolute flux-calibrated Gaia spectrum is shown in gray and shown in detail in the inset plot. The SED of the faint companion star, TOI-1450B, is shown as the lower black curve atop its broadband photometric measurements (red symbols).
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: Top: ASAS-SN V- and g-band photometry of TOI-1450, normalized to unit mean flux. Bottom: 1 day binned WASP photometry of TOI-1450.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: The crowding around TOI-1450. The sky, as seen by TESS in sector 14, is shown, with the specific aperture mask used marked in red. The star studied in this paper is marked with a white “×,” while nearby stars (identified via Gaia) are shown as red circles, with their size representative of their G magnitude relative to TOI-1450A. Only stars with a Δm  G  ≤ 6 are shown, as the brightest stars contribute maximally to the light-curve flux contamination.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: The MAROON-X RV observations of TOI-1450 with calibrated offsets between runs applied when available (and mean subtractions otherwise). The red-channel data are plotted in red, while the blue-channel data are plotted in blue.
Paper: Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A
Authors: Madison Brady, Jacob L. Bean, Andreas Seifahrt, David Kasper, Rafael Luque, Guđmundur Stefánsson, Julian Stürmer, David Charbonneau, Karen A. Collins, John P. Doty, Zahra Essack, Akihiko Fukui, Ferran Grau Horta, Christina Hedges, Coel Hellier, Jon M. Jenkins, Norio Narita, Samuel N. Quinn, Avi Shporer, Richard P. Schwarz, Sara Seager, Keivan G. Stassun, Stephanie Striegel, Cristilyn N. Watkins, Joshua N. Winn, Roberto Zambelli
Figure caption: The interferometric temperatures of the calibrator stars compared to the MAROON-X estimations.
Paper: Accurate and Model-independent Radius Determination of Single FGK and M Dwarfs Using Gaia DR3 Data
Authors: Rocio Kiman, Timothy D. Brandt, Jacqueline K. Faherty, Mark Popinchalk
Figure caption: We compared the radius estimations using our method with two samples from the literature to asses the accuracy of our method. The two samples are a set of M dwarfs from Mann et al. (2015; left panel) and a sample of FGK and M dwarfs from the Planetary Systems Composite Parameters Table from the NASA Exoplanet Archive (right panel). We color-coded the stars in each panel by the metallicities provided by each source. We included in the bottom panels the fractional radius difference as a function of the radius in the literature. In these panels a horizontal black line shows zero difference, and blue dashed lines show the median, 16th, and 84th percentiles, which are also included as blue numbers in the panel. We found good agreement between the measurements.
Paper: Accurate and Model-independent Radius Determination of Single FGK and M Dwarfs Using Gaia DR3 Data
Authors: Rocio Kiman, Timothy D. Brandt, Jacqueline K. Faherty, Mark Popinchalk
Figure caption: Comparison of the radius measurements using our Gaia SBCR and the radii in the Gaia DR3 catalog for the 50 pc sample. We show in this figure only the radii calculated by Gaia with the GSP-Phot method, and we color-coded the stars by the model used in this calculation. In general we found that our radius estimations are systematically smaller than the values in the Gaia catalog, and that the shift is different according to the model used and the radius. We found that for radius >0.6 R ⊙, the systematic difference is 3%–4% for the MARCS and A star models, but the difference is slightly smaller (2%) using the PHOENIX models. For the M dwarfs (radius <0.6 R ⊙) the offset is between 10% and 25% for GSP-Phot using PHOENIX, 7% for the MARCS models, and 13% for the FLAME method using GSP-Phot parameters.
Paper: JWST-TST DREAMS: Nonuniform Dayside Emission for WASP-17b from MIRI/LRS
Authors: Daniel Valentine, Hannah R. Wakeford, Ryan C. Challener, Natasha E. Batalha, Nikole K. Lewis, David Grant, Elijah Mullens, Lili Alderson, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Néstor Espinoza, Ana Glidden, Amélie Gressier, Jingcheng Huang, Zifan Lin, Douglas Long, Dana R. Louie, Mark Clampin, Marshall Perrin, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Gaussian significance test on the unidentified spectral features in both the ExoTiC-MIRI (left) and Eureka! (right) spectra between 9 and 12 μm. The data have the PICASO forward models presented in Figure 3 subtracted in order to fit for deviations from the modeled physics. The orange line is a flat linear fit, which would be consistent with no additional features, while the green line incorporates Gaussian fits to potentially unmodeled spectral features.
Paper: Accurate and Model-independent Radius Determination of Single FGK and M Dwarfs Using Gaia DR3 Data
Authors: Rocio Kiman, Timothy D. Brandt, Jacqueline K. Faherty, Mark Popinchalk
Figure caption: Results for our calibration of the Gaia SBCR. We show all the possible combinations between the fluxes (Equation (5)) for the three Gaia magnitudes and the three Gaia colors. We color-coded the calibration sample with metallicity, which covers the range −2.44 < [Fe/H] < 0.39 dex. We included 100 random samples of the fit for three metallicities color-coded using the same scale as shown in the color bar: [Fe/H] = −0.5, 0, 0.1. Finally we included the fitted parameters for each case, which are also shown in Table 1.
Paper: Accurate and Model-independent Radius Determination of Single FGK and M Dwarfs Using Gaia DR3 Data
Authors: Rocio Kiman, Timothy D. Brandt, Jacqueline K. Faherty, Mark Popinchalk
Figure caption: Grid plot of the posterior distributions for the four parameters of the likelihood in Equation (7) (a, b, c, and d) obtained with an MCMC fit using emcee for the case S G and (G BP − G RP).
Paper: Accurate and Model-independent Radius Determination of Single FGK and M Dwarfs Using Gaia DR3 Data
Authors: Rocio Kiman, Timothy D. Brandt, Jacqueline K. Faherty, Mark Popinchalk
Figure caption: Fractional radius difference between our radius estimation using the published Gaia photometry and the median of all the photometric points taken by Gaia for each star. We included the 1σ and 2σ deviations to show what the radius difference could be if Gaia were to take only one photometry point per star. These stars are from the Pleiades cluster (120 Myr) so we expect high photometric variability. Given that Gaia averages several photometry points to estimate the photometry of the star, photometric variability it is not an issue when estimating radii using Gaia photometry.
Paper: Accurate and Model-independent Radius Determination of Single FGK and M Dwarfs Using Gaia DR3 Data
Authors: Rocio Kiman, Timothy D. Brandt, Jacqueline K. Faherty, Mark Popinchalk
Figure caption: Color–magnitude diagram of the JMDC catalog after our quality cuts, color-coded by the literature metallicities [Fe/H]. The distribution of metallicities for our sample is shown in the inset. We also included in light gray the 100 pc sample from Gaia DR3 for comparison. We obtained the 100 pc sample from the Gaia archive applying a cut in parallax, together with a quality cut of value over error >50 for parallax and fluxes in the three Gaia bands.
Paper: Accurate and Model-independent Radius Determination of Single FGK and M Dwarfs Using Gaia DR3 Data
Authors: Rocio Kiman, Timothy D. Brandt, Jacqueline K. Faherty, Mark Popinchalk
Figure caption: Comparison of the results of estimating radii for the JMDC sample using our Gaia SBCR against the results using two recent SBCRs from Graczyk et al. (2021) and Salsi et al. (2021) for the (G − K s) color and S G. We color-coded the sample with literature metallicities. In the bottom panels we show the fractional radius difference with three horizontal blue dashed lines that show the median, 16th, and 84th percentiles, which are also included as blue numbers in each panel.
Paper: Haro 5-2: A New Pre-main-sequence Quadruple Stellar System
Authors: Bo Reipurth, C. Briceño, T. R. Geballe, C. Baranec, S. Mikkola, A. M. Cody, M. S. Connelley, C. Flores, B. A. Skiff, J. D. Armstrong, N. M. Law, R. Riddle
Figure caption: Left: example of chaotic transformation of a nonhierarchical system of four single stars into a temporary 2+2 quadruple (black/red + blue/green), which subsequently breaks up into a binary (black/red) and two single stars (blue and green). Right: example of a nonhierarchical configuration of two primordial binaries (2 and 3) that bind to form a stable 2+2 quadruple system, as an interloper flies by and carries away the excess energy. The formation of a quadruple system is far simpler when the binaries have formed prior to their interaction. Both simulations show the dynamical interactions of point sources without any gas.
Paper: High-resolution Dayside Spectroscopy of WASP-189 b: Detection of Iron during the GHOST/Gemini South System Verification Run
Authors: Emily K. Deibert, Adam B. Langeveld, Mitchell E. Young, Laura Flagg, Jake D. Turner, Peter C. B. Smith, Ernst J. W. de Mooij, Ray Jayawardhana, Kristin Chiboucas, Roberto Gamen, Christian R. Hayes, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Vinicius M. Placco, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, David O. Jones, Kathleen Labrie, Susan Ridgway, Joanna Thomas-Osip
Figure caption: Left: the Fe model used in our analysis, generated with petitRADTRANS (Mollière et al. 2019) as described in Section 4.1. The full GHOST wavelength range is displayed; however, we note that we only used a subset of this wavelength range in our analysis, indicated by the blue region (see Section 2.2). Right: the two-point T–P profile used to generate the model, using the best-fit parameters from Yan et al. (2020) and the planetary parameters listed in Table 2.
Paper: High-resolution Dayside Spectroscopy of WASP-189 b: Detection of Iron during the GHOST/Gemini South System Verification Run
Authors: Emily K. Deibert, Adam B. Langeveld, Mitchell E. Young, Laura Flagg, Jake D. Turner, Peter C. B. Smith, Ernst J. W. de Mooij, Ray Jayawardhana, Kristin Chiboucas, Roberto Gamen, Christian R. Hayes, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Vinicius M. Placco, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, David O. Jones, Kathleen Labrie, Susan Ridgway, Joanna Thomas-Osip
Figure caption: The results of cross-correlating our observations with the all-species model. Left three panels: the 2D K  p –RV maps for the blue, red, and combined results, respectively, with the location of the peak correlation signal indicated in each case by white dashed lines. The color bars indicate the significances of the maps, determined via dividing out the standard deviation away from the peak signal (see Section 4.3). A correlation signal is visible near the expected planetary location in all cases, though significantly stronger in the red than the blue. Right: slices of the 2D K  p –RV maps at the peak K  p  for the blue (blue line), red (red line), and combined (black line) results. The SNR is the same as that indicated by the color bars. The dashed black line indicates the peak RV of the combined results.
Paper: High-resolution Dayside Spectroscopy of WASP-189 b: Detection of Iron during the GHOST/Gemini South System Verification Run
Authors: Emily K. Deibert, Adam B. Langeveld, Mitchell E. Young, Laura Flagg, Jake D. Turner, Peter C. B. Smith, Ernst J. W. de Mooij, Ray Jayawardhana, Kristin Chiboucas, Roberto Gamen, Christian R. Hayes, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Vinicius M. Placco, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, David O. Jones, Kathleen Labrie, Susan Ridgway, Joanna Thomas-Osip
Figure caption: An example GHOST spectrum after reduction by the GHOST data-reduction software but prior to any additional reduction undertaken for our analyses. The blue and red arms of the data are colored in blue and red, with regions excluded from our analysis (see Section 2.2) colored in gray. Although edge orders are excluded from both detectors near 530 nm, the overlap in the detectors’ wavelength coverage means that we still have continuous coverage in our analysis.
Paper: High-resolution Dayside Spectroscopy of WASP-189 b: Detection of Iron during the GHOST/Gemini South System Verification Run
Authors: Emily K. Deibert, Adam B. Langeveld, Mitchell E. Young, Laura Flagg, Jake D. Turner, Peter C. B. Smith, Ernst J. W. de Mooij, Ray Jayawardhana, Kristin Chiboucas, Roberto Gamen, Christian R. Hayes, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Vinicius M. Placco, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, David O. Jones, Kathleen Labrie, Susan Ridgway, Joanna Thomas-Osip
Figure caption: The peak signal-to-noise ratio (SNR) of the ΔCCF map for SYSREM iterations varying from one to 20. The results for the red arm are indicated by red squares, while the results for the blue arm are indicated by blue circles. The values have been normalized to the maximum SNR of all iterations for each arm. We found that the peak SNR of the ΔCCF map corresponded to six SYSREM iterations in the red and eight SYSREM iterations in the blue. Beyond these values, the SNR steadily decreases, likely because the algorithm has begun to remove the planetary signal.
Paper: High-resolution Dayside Spectroscopy of WASP-189 b: Detection of Iron during the GHOST/Gemini South System Verification Run
Authors: Emily K. Deibert, Adam B. Langeveld, Mitchell E. Young, Laura Flagg, Jake D. Turner, Peter C. B. Smith, Ernst J. W. de Mooij, Ray Jayawardhana, Kristin Chiboucas, Roberto Gamen, Christian R. Hayes, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Vinicius M. Placco, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, David O. Jones, Kathleen Labrie, Susan Ridgway, Joanna Thomas-Osip
Figure caption: The change in air mass (top panel) and signal-to-noise ratio (SNR, bottom panel) throughout the observations. The SNR is plotted separately for the blue and red arms of the instrument, and is the average SNR per pixel per exposure across all orders. The SNR appears to decrease with increasing air mass at the end of our observations, as expected. The ∼20 minutes gap in our observing coverage is visible.
Paper: High-resolution Dayside Spectroscopy of WASP-189 b: Detection of Iron during the GHOST/Gemini South System Verification Run
Authors: Emily K. Deibert, Adam B. Langeveld, Mitchell E. Young, Laura Flagg, Jake D. Turner, Peter C. B. Smith, Ernst J. W. de Mooij, Ray Jayawardhana, Kristin Chiboucas, Roberto Gamen, Christian R. Hayes, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Vinicius M. Placco, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, David O. Jones, Kathleen Labrie, Susan Ridgway, Joanna Thomas-Osip
Figure caption: A visualization of the post-eclipse orbital phases (∼0.58 to ∼0.63) covered by these observations. The planetary orbit and host star are drawn to scale. Note that the brief gap in our observations is not visible, but can be seen in Figure 2.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Modeled PCs P r(λ) of cometary dust. Columns left and right show modeled results for dust with wavelength-dependent and wavelength-independent imaginary parts of the refractive index (m i), respectively. The color scheme in the left column follows that of Figure 13 to distinguish cases with different m i, while the colors used in the right column are given in the legend. Each row presents PC for different p-values, compared with the observed results at three epochs (red diamonds). As in Figure 13, we omitted the result of p = 5.0 due to its similarity to that of p = 4.5.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Modeled polarization-phase curves P r(α) of cometary dust. Presented are the modeled distributions of dust particles with different power-law indices p in the Red (left column) and I-filter (right column) domains. Each row shows observations acquired for each epoch of polarimetry. A solid horizontal line with colored areas indicates a P r value and its 1σ uncertainty. Each line of colored circles representing different imaginary parts of the refractive indices m i (labeled in the legend) stamps modeled P r at a given p. The case of p = 5.0 is not present here due to its almost identical result to p = 4.5.