adsabs/AstroCLIMB huggingface dataset:
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: Constraining the slope of ratioed density trends with varying sample sizes. The y-values correspond to the slope of the scaled density (ρ/ρ⊕,s) as a function of equilibrium temperature (Teq) (Mp), which is positive when considering the full sample of 104 simulated planets. Panel (1) corresponds to the upper-limit estimate of the transit radius, where the atmosphere has two layers and Ptransit = 10−6 bar, while panel (2) represents the lower-limit estimate, where the atmosphere has three layers and Ptransit = 0.02 bar. The solid lines indicate the median slope values derived from bootstrap resampling, while the shaded regions represent the 90% confidence intervals. Different colors represent assumptions for solid-body density: (a, blue) fixed Earth-like composition; (b, red) Gaussian scatter with σ = 1/3 the difference between pure-silicate and Earth-like; (c, yellow) wider Gaussian with σ = full silicate–Earth difference. The results illustrate how increasing the sample size improves the precision of the slope estimation. The wiggles are artifacts of the Monte Carlo procedure.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: Upper panel: escape rate at high-XUV plateau of N2-dominated atmospheres as a function of planetary mass, based on R. D. Chatterjee & R. T. Pierrehumbert (2024). The right y-axis represents the total atmospheric loss over 3 Gyr, which also defines the critical initial volatile content required for atmospheric retention over this timescale-planets with an initial volatile mass above this threshold can retain their atmosphere regardless of past XUV flux intensity. Lower panel: the critical initial volatile fraction (relative to planetary mass) (﹩{f}_{\mathrm{initial}}^{* }﹩) sufficient to sustain an atmosphere over 3 Gyr, independent of historical XUV flux intensity, shown as a function of planetary mass. The shaded region represents uncertainty in the critical flux at which the escape rate plateaus (see Table 1).
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: A subset of the burst waterfalls from the repeating sources in our sample. Each burst is de-dispersed to its structure maximizing DM, with the relevant fitburst fit shown on top of the burst. The time resolution at which the burst is displayed is listed in the top-right corner. The dashed, white lines indicated the derived bandwidth range for the source. Channels that were masked due to RFI are shown in dark green/teal. The repeater name is shown in the top-left corner, while the individual burst name is listed at the top.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: The same as Figure 4 except limiting the burst to those studied at time resolutions ≤40 μs.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Bandwidth versus detection S/N for all sources in our sample for which there are more than five bursts with the complex raw voltages recorded. The color scale indicates the log of the spectral fluence over the spectral extent of the burst.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: The same as bottom-right panel of Figure 1 except including nonrepeating FRBs from K. R. Sand et al. (2024).
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: The same as top-left panel of Figure 1 except using the maximum burst duration per repeating FRB source.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: The same as bottom-left panel of Figure 1 except including nonrepeating FRBs from K. R. Sand et al. (2024).
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: The same as Figure 7 except for FRB 20200929C.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: The same as Figure 8 except for FRB 20191106C.
Paper: Turbulent Magnetic Fields and Molecular Cloud Interactions in the Supernova Remnant G1.9+0.3
Authors: Moeri Tao, Takaaki Tanaka, Hidetoshi Sano, Rami Z. E. Alsaberi, Jun Kataoka
Figure caption: (a) Two-color image of G1.9+0.3: Chandra X-ray data are shown in blue, and the 9 GHz radio data (obtained with ATCA) are shown in red (R. Enokiya et al. 2023). The overlaid contour represents the integrated intensity distribution of the associated cloud in 12CO(J = 3–2). The contour levels of CO are 25.000, 28.125, 31.250, 34.375, 37.500, 40.625, 43.750, 46.875, and 50.000 K km s−1. (b) Exposure-corrected Chandra X-ray image (0.5−7.0 keV) from 2011 observations. The solid green line marks the source region (entire remnant), and the dotted green line indicates the background region. (c) Same as (b) but showing source regions for NE, North, NW, SW, South, and SE sectors (outlined in solid green). The color scale represents flux in units of count s−1. Both images are smoothed using a Gaussian kernel with σ = 1″5 . White crosshairs indicate reference axes for the azimuthal profile shown in Figure 3, aligned with Galactic longitude and latitude.
Paper: Turbulent Magnetic Fields and Molecular Cloud Interactions in the Supernova Remnant G1.9+0.3
Authors: Moeri Tao, Takaaki Tanaka, Hidetoshi Sano, Rami Z. E. Alsaberi, Jun Kataoka
Figure caption: Azimuthal profiles of G1.9+0.3, centered at (l, b) = (1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩8710, 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩3237) (see Figure 1). Black points represent the spatial variation of the Bohm factor η. The gray shaded area shows the integrated 12CO(J = 3–2) flux density, while the region marked by the blue line shows the integrated 9 GHz radio flux density (based on Figure 9 from R. Enokiya et al. 2023).
Paper: Turbulent Magnetic Fields and Molecular Cloud Interactions in the Supernova Remnant G1.9+0.3
Authors: Moeri Tao, Takaaki Tanaka, Hidetoshi Sano, Rami Z. E. Alsaberi, Jun Kataoka
Figure caption: SED of G1.9+0.3 as a whole. Radio data (orange open circles) were compiled from D. Green et al. (2008) and K. J. Luken et al. (2020). The HESS upper limits are shown for two spectral indices: 2.0 (red curve) and 3.0 (blue curve) from HESS Collaboration et al. (2014). The green curve corresponds to synchrotron emission from regions with amplified magnetic fields, while the magenta curves represent synchrotron and IC on CMB emission fitted modeled for the lower-limit field strength B = 12 μG as derived in HESS Collaboration et al. (2014).
Paper: Turbulent Magnetic Fields and Molecular Cloud Interactions in the Supernova Remnant G1.9+0.3
Authors: Moeri Tao, Takaaki Tanaka, Hidetoshi Sano, Rami Z. E. Alsaberi, Jun Kataoka
Figure caption: Relationship between the shock velocity and cutoff energy with equi-η curves: η = 1, 2, 3, 4, 5, 10, and 15 (Equation (4)).
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: Our MBH estimate for NGC 7052 in the context of various MBH–σ scaling relations and their intrinsic scatters.
Paper: A Novel Approach to Identifying Substructures through Analysis of Metallicity Distribution Functions
Authors: Young Kwang Kim, Young Sun Lee, 영선 이, Timothy C. Beers
Figure caption: Top: distribution of ED-2 stars in e vs. [Fe/H]. Red circles represent the ED-2 candidates from our sample; the stars with e ≤ 0.5 among them are plotted as black open squares. The ED-2 members from high-resolution spectroscopic observations of E. Balbinot et al. (2024) are shown with green circles; the stars with e ≤ 0.5 are displayed as black open triangles. The ED-2_DESI sample with e > 0.5 from B. Kim et al. (2025) is marked with black circles. The single ED-2 member added by E. Balbinot et al. (2023) is shown as an orange star. An orange cross indicates the Gaia BH 3 companion star from Gaia Collaboration et al. (2024). Middle panel: same as in the top panel, but in rapo vs. [Fe/H]. Bottom panel: MDFs of our ED-2 candidates, the ED-2 members, and the ED-2_DESI sample with e > 0.5. The MDFs of the ED-2 candidates with e > 0.5 from our sample are shown with solid red lines; solid orange lines are those with e ≤ 0.5. Similarly, the MDFs of the ED-2 members with e > 0.5 from high-resolution spectroscopic observations of E. Balbinot et al. (2024) are shown with solid green lines; dashed green lines are those with e ≤ 0.5. The MDF of the ED-2_DESI sample with e > 0.5 from B. Kim et al. (2025) is shown with a dashed black line. The black dotted vertical lines are the MDF peaks for the ED-2 members with e > 0.5, our ED-2 candidates with e > 0.5, and our ED-2 candidates with e ≤ 0.5.
Paper: A Novel Approach to Identifying Substructures through Analysis of Metallicity Distribution Functions
Authors: Young Kwang Kim, Young Sun Lee, 영선 이, Timothy C. Beers
Figure caption: Left panels: the differences between dPZ26 and d, as a function of d, and the differences between the eccentricities obtained at those different distance scales, as a function of e, for the PZ26 sample. Right panels: same as the left panels, but for the SH sample. Magenta circles are stars whose orbital eccentricities are within the selected range of eccentricities for both distance scales, but whose orbital inclinations obtained at this study’s distance are outside the chosen range of orbital inclinations. All black circles between the two blue vertical lines, excluding the magenta circles, are stars in common with the kinematic–orbital selection space for both distance scales.
Paper: A Novel Approach to Identifying Substructures through Analysis of Metallicity Distribution Functions
Authors: Young Kwang Kim, Young Sun Lee, 영선 이, Timothy C. Beers
Figure caption: Same as Figure 7, but for the PZ26 sample (left panels) and for the SH sample (right panels). For each of the left and right panels, the numbers in parentheses are the number of stars in common with the result from this study’s distance for each substructure in the PZ26 sample and in the SH sample.
Paper: COSMOS-Web: MIRI Data Reduction and Number Counts at 7.7 μm Using JWST
Authors: Santosh Harish, Jeyhan S. Kartaltepe, Daizhong Liu, Anton M. Koekemoer, Caitlin M. Casey, Maximilien Franco, Hollis B. Akins, Olivier Ilbert, Marko Shuntov, Nicole E. Drakos, Mike Engesser, Andreas L. Faisst, Ghassem Gozaliasl, Crystal L. Martin, Michaela Hirschmann, Vasily Kokorev, Erini Lambrides, Henry Joy McCracken, Jed McKinney, Louise Paquereau, Jason Rhodes, Brant E. Robertson
Figure caption: Cumulative number counts at 7.7 μm from COSOMS-Web in comparison with model predictions (left) and other JWST and IRAC number counts from the literature (right). Uncertainties for the COSMOS-Web number counts are a combination of Poisson and cosmic variance errors added in quadrature. The dotted vertical line in each panel represents the average 5σ limiting depth achieved in the COSMOS-Web MIRI observations, and also corresponds to the 80% completeness limit as mentioned in Section 4.3. In the left panel, we compare our source counts with a number of model predictions at 8 μm including those based on the semianalytical models GALFORM+GRASIL (W. I. Cowley et al. 2018) and SHARK (C. d. P. Lagos et al. 2019), the SPRITZ simulations (L. Bisigello et al. 2021), and the semiempirical models of M. Rowan-Robinson (2009, 2024) and V. I. Kokorev et al. (2021). We also compare our number counts with estimates from recent JWST (MIRI F770W) studies including the CEERS (G. Yang et al. 2023), JADES, and SMILES (M. A. Stone et al. 2024) programs, as well as Spitzer (IRAC CH4) counts from the SDWFS (M. L. N. Ashby et al. 2009) program.
Paper: COSMOS-Web: MIRI Data Reduction and Number Counts at 7.7 μm Using JWST
Authors: Santosh Harish, Jeyhan S. Kartaltepe, Daizhong Liu, Anton M. Koekemoer, Caitlin M. Casey, Maximilien Franco, Hollis B. Akins, Olivier Ilbert, Marko Shuntov, Nicole E. Drakos, Mike Engesser, Andreas L. Faisst, Ghassem Gozaliasl, Crystal L. Martin, Michaela Hirschmann, Vasily Kokorev, Erini Lambrides, Henry Joy McCracken, Jed McKinney, Louise Paquereau, Jason Rhodes, Brant E. Robertson
Figure caption: Photometric comparison of MIRI F770W detections with IRAC CH4 measurements from the COSMOS2020 catalog. For the sake of accuracy, we compare MIRI photometry with IRAC CH4 only for sources with S/NCH4 ≥ 5 and magCH4 ≤ 22.3 in the COSMOS2020 catalog (brown-black points). Left panel: a 1:1 comparison with the identity line (diagonal dashed–dotted line) and the 5σ limiting depth for IRAC CH4 (horizontal dotted line) shown for reference. For the matched sample, the magnitude offset (Δmag = F770W − CH4) as a function of the MIRI F770W photometry is shown in the right panel. Also shown are median offsets per magnitude bin (orange-red squares) derived by binning sources based on their MIRI F770W photometry along with their 3σ-clipped standard deviation. Some of the bins at the bright end (mF770W < 19.5) have asymmetric widths because we required each bin to contain a minimum of 10 sources.
Paper: COSMOS-Web: MIRI Data Reduction and Number Counts at 7.7 μm Using JWST
Authors: Santosh Harish, Jeyhan S. Kartaltepe, Daizhong Liu, Anton M. Koekemoer, Caitlin M. Casey, Maximilien Franco, Hollis B. Akins, Olivier Ilbert, Marko Shuntov, Nicole E. Drakos, Mike Engesser, Andreas L. Faisst, Ghassem Gozaliasl, Crystal L. Martin, Michaela Hirschmann, Vasily Kokorev, Erini Lambrides, Henry Joy McCracken, Jed McKinney, Louise Paquereau, Jason Rhodes, Brant E. Robertson
Figure caption: Astrometric offsets between MIRI F770W detections (S/N ≥ 5) and their HST/ACS F814W counterparts, which are aligned to Gaia DR3, assuming a cross-match radius of 1″. Shown for reference are dashed circles with radii 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩1, 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2, and 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩3 centered on (0, 0), depicting the relative positional offsets of all MIRI sources. The median offsets in R.A. and decl. are 0.35 and 6 mas respectively (MIRI native pixel scale is 110 mas) with a median absolute deviation of 28 mas in both directions.
Paper: COSMOS-Web: MIRI Data Reduction and Number Counts at 7.7 μm Using JWST
Authors: Santosh Harish, Jeyhan S. Kartaltepe, Daizhong Liu, Anton M. Koekemoer, Caitlin M. Casey, Maximilien Franco, Hollis B. Akins, Olivier Ilbert, Marko Shuntov, Nicole E. Drakos, Mike Engesser, Andreas L. Faisst, Ghassem Gozaliasl, Crystal L. Martin, Michaela Hirschmann, Vasily Kokorev, Erini Lambrides, Henry Joy McCracken, Jed McKinney, Louise Paquereau, Jason Rhodes, Brant E. Robertson
Figure caption: Exposure map of completed MIRI visits from the COSMOS-Web program. Shown for reference are (a) the HST ACS F814W mosaic outline (maroon) of the COSMOS field (A. M. Koekemoer et al. 2007; N. Scoville et al. 2007), (b) the overall COSMOS-Web NIRCam mosaic outline as well as the tiles layout (blue; M. Franco et al. 2025), and (c) the PRIMER MIRI coverage (red; JWST GO PID 1837).
Paper: COSMOS-Web: MIRI Data Reduction and Number Counts at 7.7 μm Using JWST
Authors: Santosh Harish, Jeyhan S. Kartaltepe, Daizhong Liu, Anton M. Koekemoer, Caitlin M. Casey, Maximilien Franco, Hollis B. Akins, Olivier Ilbert, Marko Shuntov, Nicole E. Drakos, Mike Engesser, Andreas L. Faisst, Ghassem Gozaliasl, Crystal L. Martin, Michaela Hirschmann, Vasily Kokorev, Erini Lambrides, Henry Joy McCracken, Jed McKinney, Louise Paquereau, Jason Rhodes, Brant E. Robertson
Figure caption: Normalized photometric redshift distribution of the 7.7 μm MIRI-selected sources from the COSMOS-Web catalog. Left: redshift distribution for the subsamples based on two different brightness thresholds. The bright end (mF770W < 22) is dominated by low-redshift sources (z < 2) whereas higher-redshift sources (z > 2) become more prevalent as we move toward the faint end. Right: redshift distribution for the subsamples based on the source classification from LePHARE measurements. Each source class is normalized independently to highlight relative redshift distributions.
Paper: COSMOS-Web: MIRI Data Reduction and Number Counts at 7.7 μm Using JWST
Authors: Santosh Harish, Jeyhan S. Kartaltepe, Daizhong Liu, Anton M. Koekemoer, Caitlin M. Casey, Maximilien Franco, Hollis B. Akins, Olivier Ilbert, Marko Shuntov, Nicole E. Drakos, Mike Engesser, Andreas L. Faisst, Ghassem Gozaliasl, Crystal L. Martin, Michaela Hirschmann, Vasily Kokorev, Erini Lambrides, Henry Joy McCracken, Jed McKinney, Louise Paquereau, Jason Rhodes, Brant E. Robertson
Figure caption: Completeness fraction as a function of MIRI F770W flux. The uncertainties (shaded region) shown here are purely Poisson errors. The 80% completeness limit (horizontal dashed line) as well as the median 5σ limiting depth (vertical dotted line), including the 1σ scatter (gray shaded region), are shown for reference. Our MIRI source sample achieves ≥80% completeness for all sources detected with S/N ≥ 5σ.
Paper: COSMOS-Web: MIRI Data Reduction and Number Counts at 7.7 μm Using JWST
Authors: Santosh Harish, Jeyhan S. Kartaltepe, Daizhong Liu, Anton M. Koekemoer, Caitlin M. Casey, Maximilien Franco, Hollis B. Akins, Olivier Ilbert, Marko Shuntov, Nicole E. Drakos, Mike Engesser, Andreas L. Faisst, Ghassem Gozaliasl, Crystal L. Martin, Michaela Hirschmann, Vasily Kokorev, Erini Lambrides, Henry Joy McCracken, Jed McKinney, Louise Paquereau, Jason Rhodes, Brant E. Robertson
Figure caption: Photometric comparison between SE++ model magnitudes and SE AUTO aperture magnitudes for MIRI F770W. The median offset along with the 3σ-clipped standard deviation is shown by the white dashed lines. Also shown for reference are the ±1σ and ±3σ photometric uncertainties (cyan dotted lines) combined in quadrature from the two photometric measurements.
Paper: COSMOS-Web: MIRI Data Reduction and Number Counts at 7.7 μm Using JWST
Authors: Santosh Harish, Jeyhan S. Kartaltepe, Daizhong Liu, Anton M. Koekemoer, Caitlin M. Casey, Maximilien Franco, Hollis B. Akins, Olivier Ilbert, Marko Shuntov, Nicole E. Drakos, Mike Engesser, Andreas L. Faisst, Ghassem Gozaliasl, Crystal L. Martin, Michaela Hirschmann, Vasily Kokorev, Erini Lambrides, Henry Joy McCracken, Jed McKinney, Louise Paquereau, Jason Rhodes, Brant E. Robertson
Figure caption: The COSMOS-Web MIRI F770W mosaic. The zoomed-in areas show 45″ × 45″ matched regions in both MIRI F770W and IRAC CH4 from different parts of the mosaic. These cutouts highlight the significant improvement in sensitivity (∼50×) and resolution (∼7×) of MIRI observations compared to IRAC. The montage of cutouts is shown with the same stretch for direct comparison.
Paper: COSMOS-Web: MIRI Data Reduction and Number Counts at 7.7 μm Using JWST
Authors: Santosh Harish, Jeyhan S. Kartaltepe, Daizhong Liu, Anton M. Koekemoer, Caitlin M. Casey, Maximilien Franco, Hollis B. Akins, Olivier Ilbert, Marko Shuntov, Nicole E. Drakos, Mike Engesser, Andreas L. Faisst, Ghassem Gozaliasl, Crystal L. Martin, Michaela Hirschmann, Vasily Kokorev, Erini Lambrides, Henry Joy McCracken, Jed McKinney, Louise Paquereau, Jason Rhodes, Brant E. Robertson
Figure caption: Example MIRI F770W image based on the default pipeline output (left) and the same with our master background subtraction procedure applied (right) as detailed in Section 3.3. The stretch in both images is the same.