adsabs/AstroCLIMB huggingface dataset:
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The top panel shows the results of the maximum-likelihood solution for NGC 6958. The abscissa is the galaxy’s true distance modulus, the ordinate is α 2.5, the number of PNe within 2.5 mag of M*, normalized to the amount of bolometric light sampled. The contours are drawn at 0.5σ intervals. The bottom panel marginalizes this distribution over the PN/light variable. The low value of α 2.5 is most likely due to incompleteness in our survey.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The observed PNLF for NGC 6958 binned into 0.25 mag intervals. Although incompleteness likely affects our entire survey, we only consider PNe brighter than m 5007 = 29.2 in our fit. Fainter objects are denoted by open circles. The error bars illustrate the uncertainties of small number counting statistics (Gehrels 1986). The curve shows Equation (2) shifted by the best-fit apparent distance modulus of (m − M)0 = 32.80.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The cumulative luminosity function for PNe in NGC 5248. The dark line shows the observed data and the curve is Equation (2) shifted to the most likely apparent distance modulus of (m − M)0 = 31.93. The dark red line shows PN1 and the dashed line denotes where incompleteness begins to affect the detections. Data brighter than this are consistent with being drawn from the empirical function. A K-S test excludes the inclusion of PN1 at the 99% confidence level.
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The results of the maximum-likelihood analysis for NGC 5248. The abscissa is the galaxy’s true distance modulus, the ordinate the relative likelihood of the solution. PN1 has been excluded from the analysis. This distance is consistent with the Tully–Fisher-based estimate of Ekholm et al. (2000).
Paper: Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data
Authors: George H. Jacoby, Robin Ciardullo, Martin M. Roth, Magda Arnaboldi, Peter M. Weilbacher
Figure caption: The top panel shows the results of the maximum-likelihood solution for NGC 4472. The abscissa is the galaxy’s true distance modulus, the ordinate is α 2.5, the number of PNe within 2.5 mag of M*, normalized to the amount of bolometric light sampled. The contours are drawn at 0.5σ intervals. The bottom panel marginalizes this distribution over the PN/light variable.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Observationally deduced fractional abundances (f), relative to H2, of all the λ 3 mm band detected species (X) toward IRC+10216 by the PMO 13.7 m telescope, as a function of radius (R). In the plot, f(X) = N(X)/N  R (H2), where N(X) depict the total column density of the species (X), and N  R (H2) (the red dashed–dotted line) represents the beam-averaged H2 column density at radius R. Except for CO and 13CO, the detected molecules are located within the area marked by the gray-dashed lines.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Illustrations for the impact of the employed source size (θ  s ) on the calculated excitation temperature (T ex) and column density (N) of HC5N (in red), CN (in blue), and SiO (in green).
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: 84.5–115.8 GHz spectrum of IRC+10216 displayed in consecutive 475 MHz frequency segments with 0.244 MHz spectral resolution.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Same as Figure 2 but for C2H and I-C3H. The solid blue line indicates the hfs components of the molecule. The rest frequencies in MHz are shown in each panel’s upper right corner for single structure components, and in the upper left and right corners for lines with two fine structure components.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Same as Figures 2 and C1 but for C2H, C4H(ν = 1), C2S and CN. The blue-dashed lines represent the blended spectral lines.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Same as Figures 2 and C1 but for CN. The rest frequencies in MHz of spectral lines of more than two fine structure components are displayed in the upper left corner of each panel.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Same as Figure 2 but for C4H.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Same as Figure 2 but for C3N and c-C3H2.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Same as Figures 2 and C3 but for HC3N, and its isotopologues.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Same as Figure 2 but for HC5N.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Multicomponents revealed in the rotational diagrams of several species: HC3N, HC5N, C3S, C4H  (ν = 0), C4H  (ν = 1), and CH3CN. The results obtained from the linear least squares fitting are plotted in black-dashed lines. The adopted data points with error bars are from our PMO 13.7 m observations (black triangles), He et al. (2008) (blue triangles), Gong et al. (2015) (cyan triangles), Zhang et al. (2017) (dark orange triangles), Kawaguchi et al. (1995) (yellow-green triangles), Cernicharo et al. (2000) (red triangles), Agúndez et al. (2012) (green triangles), and Groesbeck et al. (1994) (magenta triangles), respectively. Note that the error bars are invisible if their values are smaller than the adopted data points.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Same as Figures 2 and C1 but for CS, 13CS, C34S, C2S, C3S, MgNC, and CH3CN.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Rotational diagrams for the identified molecules in IRC+10216 in the λ 3 mm wavelength band. The results obtained from the linear least squares fitting are plotted in black-dashed lines. The adopted data points with error bars are from our PMO 13.7 m observations (black triangles), He et al. (2008) (blue triangles), Gong et al. (2015) (cyan triangles), Zhang et al. (2017) (dark orange triangles), Kawaguchi et al. (1995) (yellow-green triangles), Cernicharo et al. (2000) (red triangles), Agúndez et al. (2012) (green triangles), and Groesbeck et al. (1994) (magenta triangles), respectively. Note that the error bars are invisible if their values are smaller than the adopted data points.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Same as Figures 2 and C1 but for HCN, H13CN, HNC, and 29SiO.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption: Same as Figure 2 but for SiS, 29SiS, Si34S and SiC2.
Paper: A λ 3 mm Line Survey toward the Circumstellar Envelope of the Carbon-rich AGB Star IRC+10216 (CW Leo)
Authors: Juan Tuo, Xiaohu Li, Jixian Sun, Tom J. Millar, Yong Zhang, Jianjie Qiu, Donghui Quan, Jarken Esimbek, Jianjun Zhou, Yu Gao, Qiang Chang, Lin Xiao, Yanan Feng, Zhenzhen Miao, Rong Ma, Ryszard Szczerba, Xuan Fang
Figure caption:                         Same as Figure E1, but for different molecular species. Note, molecular c-C3H2 is separated into ortho (open triangles) and para (filled triangles) states and fitted in solid (ortho) and dotted (para) lines. The data shown in saddle-brown triangles with error bars are obtained from Nyman et al. (1993).
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: NIRCam CMDs of M92 in select filter combinations. These CMDs exclude the third exposure. Panels (a), (b), and (c) show the CMDs for the SW (F090W−F150W), LW (F277W−F444W), and an example SW/LW (F090W−F277W) filter combination. The left side of each plot shows CMDs of all objects detected, while the right panels are CMDs of stars that passed the culling criteria. In all cases, the photometry is of excellent quality, and the culling criteria removes a large fraction of obvious nonstellar sources. There appear to be two MSs in the F090W−F277W CMD that are offset in color from one another. This is due to small zero-point differences between the NIRCam chips/modules.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: The spatial distribution of objects and stars detected by DOLPHOT in our NIRCam imaging of M92, excluding the third exposure. Left: A density map (∼50 × 50 pixel bins) of the ∼9.8 × 105 objects reported in the raw DOLPHOT catalog. There is a density gradient toward the center of the image and cluster center. Additional features include a high density of sources that trace saturated stars and a lower density of sources in the SW chip gaps. Right: The density map of stars that passed the catalog culling criteria listed in Section 3.5. These criteria removed the vast majority of obvious artifacts (e.g., corresponding to saturated stars, diffraction spikes) and reveal a clear stellar density gradient as is expected for a globular cluster. Note that the individual SW chips are labeled.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: An illustration of the effects of temporal variations on the photometry of M92. We show scatter from the S/N > 50 M92 ASTs in F150W in panel (a) as a point of comparison. The other panels show the no event case (panel (b); i.e., normal temporal variations), a small misalignment event (panel (c)), and a large misalignment event (panel (d)). Each of these panels shows the difference in F150W magnitudes of the same high-S/N stars (S/N > 50) for our fiducial photometry and photometry computed using WebbPSF models from an epoch corresponding to an event. For normal operation (panel (b)) and small misalignment events (panel (c)), there is very little difference in the photometry. For the large misalignment event, a nonnegligible amount of scatter can be present and should be included in the error budget. Large events may also impact the astrometry. See Section 5.2 and Table 6 for more details. Fortunately, such large events appear to be rare.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: An illustration of improvements in DOLPHOT NIRCam photometry since the publication of our survey paper in early 2023 demonstrated by showing F090W-F150W CMDs of M92 from various DOLPHOT runs in the past year. Panel (a) shows the CMD from our ERS survey paper (Weisz et al. 2023) from January 2023. It was constructed using all exposures of M92, including the anomalous third exposure, and used JWST calibrations and WebbPSF models from late 2022. Panel (b) shows photometry from the same time frame, only without the third exposure. Panel (c) shows the CMD of M92 (no third exposure) using the older WebbPSF models (v1.1) and calibration data, but with updated NIRCam zero-points released in fall 2023. Panel (d) shows the M92 CMD published in this paper (with no third exposure), which includes updated WebbPSF models and very recent calibrations (e.g., flat fields) and zero-points. From left to right, the CMDs have noticeably less scatter, tighter stellar CMD sequences (e.g., MSTO, MS kink), more stars, and improved depth.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: M92 SW NIRCam CMDs illustrating the effects of the anomalous third exposure. Panel (a): culled CMD based on photometry of exposures 1,2, and 4. Panel (b): culled CMD based on photometry using exposures 1,2,3, and 4. Panel (c): culled CMD of only exposure 3. A visual comparison of panels (a) and (b) shows that the inclusion of the third exposure results in more scatter in the combined CMD. This is most evident near the MSTO, which is much broader in panel (b) than in panel (a), but is also present in virtually all other regions of the CMD. The CMD of the third exposure in panel (c) shows poor photometry despite no obvious diagnostic issues raised in DOLPHOT. This pattern is present in the third exposure of the NIRISS M92 imaging. The issue appears to be a small amount of increased jitter in the telescope, as revealed by analysis of the fine guidance sensor data.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: Improvements in DOLPHOT NIRISS photometry, illustrated by CMDs of M92. Panels (a) and (b) are the NIRISS CMDs released as part of the ERS survey paper in January 2023 (Weisz et al. 2023); with the CMD constructed from four exposures shown in panel (a) and the CMD constructed without the third exposure in panel (b). Panel (c) shows the NIRISS CMD from this paper, which includes updated WebbPSF models and JWST NIRISS calibrations. It does not include the third exposure. The CMD in panel (c) has less scatter, tighter sequences, more stars, and greater depth than our previous NIRISS CMDs.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: An illustration of temporal variations in an example F150W NIRCam PSF computed using WebbPSF. Each panel shows the ratio of flux per pixel in each model PSF for a given misalignment scenario (panel (a), no event; panel (b), small event; panel (c), large event) relative to the nominal PSF. The changes to the PSF are small, but nonzero, for both the no event and small event scenarios. The large event results in substantial change to the PSF. As summarized in Table 6, time and/or alignment variations to the PSF do not appear to introduce bias into the photometry, but they do add scatter of ∼2%–10% depending on the size of the event and wavelength.