adsabs/AstroCLIMB huggingface dataset:
Paper: A Temperature Trend for Clouds and Hazes in Exoplanet Atmospheres
Authors: Raissa Estrela, Mark R. Swain, Gael M. Roudier
Figure caption: Comparison between the Jupiter’s haze profile and the scaled haze model obtained with the averaged aerosol properties found in the exoplanet sample. The thickness of Jupiter’s haze layer is shown by a solid line, and the median thickness found for the exoplanet catalog in this study is indicated by a dashed line. For the exoplanet model, we also illustrate the location of the haze peak density (in terms of pressure) in red and the cloud-top pressure (CTP), indicated by a solid line. Any atmospheric content below the CTP (within the gray region) would be muted.
Paper: A Temperature Trend for Clouds and Hazes in Exoplanet Atmospheres
Authors: Raissa Estrela, Mark R. Swain, Gael M. Roudier
Figure caption: Comparison between the retrieved Cerberus model for the target HAT-P-26b and the model without clouds and hazes used to obtain the spectral modulation index.
Paper: The Imprint of Intermittent Interchange Reconnection on the Solar Wind
Authors: Peter F. Wyper, C. R. DeVore, S. K. Antiochos, D. I. Pontin, Aleida K. Higginson, Roger Scott, Sophie Masson, Theo Pelegrin-Frachon
Figure caption: Field lines within the plasmoid flux rope highlighted with the red arrow in Figure 2(c) as it is ejected from the current layer. The field lines are colored (blue/green) according to the local plasma velocity magnitude. Note that the field lines are chosen to show the twist evolution within the flux rope and differ between times. The gray shading shows ∣J∣ as in Figure 2(a).
Paper: The Imprint of Intermittent Interchange Reconnection on the Solar Wind
Authors: Peter F. Wyper, C. R. DeVore, S. K. Antiochos, D. I. Pontin, Aleida K. Higginson, Roger Scott, Sophie Masson, Theo Pelegrin-Frachon
Figure caption: (a) Field lines showing the 3D magnetic null-point topology after the relaxation. (b) Radial profile of the relaxed state showing plasma β (solid line), v  A  (dashed), and v  r  (dotted).
Paper: What Are Those Tiny Things? A First Study of Compact Star Clusters in the SMACS0723 Field with JWST
Authors: Andreas L. Faisst, Ranga Ram Chary, Gabriel Brammer, Sune Toft
Figure caption: Properties of the compact star clusters found in the SMACS0723 field. Left panel: magnitude distribution in F090W (blue), F200W (orange), and F444W (red semifilled). The vertical gray area shows the range in 3σ limits in the three filters shown. The blue filled histogram shows the expected number of Milky Way stars from Wainscoat et al. (1992) toward the cluster field within the full NIRCam FoV. The dark blue horizontal lines show the same for the combined number of M/L/T stars from Kirkpatrick et al. (2021). Middle panel: the distribution of the extracted compact star clusters (purple circles; median as purple star) in color space. Typical errors in the colors are shown by the error bars in black (lowest 10% and median errors). The distribution of (dereddened) colors of star-forming (gray) and quiescent (red) galaxies at z = 0.39 from the COSMOS2020 catalog (Weaver et al. 2022) is shown. The star clusters match with the color distribution of the quiescent galaxy population. The A v = 2 mag extinction vector is also shown. Right panel: the 2.2 μ m magnitude vs. stellar mass relation of quiescent galaxies (red dots) is similar to the one of the star clusters, indicating a similar K-band M/L ratio. The stellar masses of the star clusters (median of ﹩{2.4}_{-1.5}^{+3.0}\,\times \,{10}^{6}\,{M}_{\odot }﹩; see inset) are derived from the M/L ratio of the best-fit SSP models (Section 3.1.3).
Paper: What Are Those Tiny Things? A First Study of Compact Star Clusters in the SMACS0723 Field with JWST
Authors: Andreas L. Faisst, Ranga Ram Chary, Gabriel Brammer, Sune Toft
Figure caption: Results from fitting the photometry of all extracted compact star clusters. Left panel: χ 2 map of the age vs. metallicity grid with 3σ, 4σ, and 5σ contours indicated. The cross marks the best-fit solution (0.2 Z ⊙ and 1.5 Gyr). The age of the universe at z = 0.39 (9.3 Gyr) is indicated by the horizontal white line. For the full globular population we find an age of ﹩{1.5}_{-0.5}^{+0.5}\,\mathrm{Gyr}﹩ and a best-fit metallicity of 20%–30% solar. Metallicities of <20% or more than solar are ruled out at high significance. Right panel: data (black symbols) and best-fit SSP model (black line) shown with other models of different age and metallicity combinations (see legend). While different metal abundances produce different SEDs at <1.5 μm, older ages are difficult to discern. Better wavelength sampling with mediumband filters at 2–3 μm and 4–4.5 μm wavelengths would constrain older ages better. The colored lines show blackbody models at different temperatures normalized to 1 μm.
Paper: What Are Those Tiny Things? A First Study of Compact Star Clusters in the SMACS0723 Field with JWST
Authors: Andreas L. Faisst, Ranga Ram Chary, Gabriel Brammer, Sune Toft
Figure caption: Upper limits on the sizes of the compact star clusters (purple) compared to sizes of z = 0.39 galaxies from HST COSMOS-DASH (Mowla et al. 2019; Cutler et al. 2022) in WFC3/F160W (light gray dots) and measured from NIRCam/F150W at lower masses (dark gray dots). The line shows a linear fit to the M–R e relation. Also indicated are typical sizes of star-forming regions in local galaxies (light blue hatched with 1σ percentile; Larson et al. 2020), the sizes/masses of dwarf galaxies around the Milky Way (black squares; Strigari et al. 2008), and sizes/masses of local globular clusters (black box; Larsen et al. 2001; Hilker et al. 2020). The z = 0.39 compact star clusters overlap with the massive end of the stellar mass distribution of local globular cluster as well as with common masses of Milky Way dwarf assuming they lose ∼90% of their mass during close passages to the BCG (black arrow).
Paper: What Are Those Tiny Things? A First Study of Compact Star Clusters in the SMACS0723 Field with JWST
Authors: Andreas L. Faisst, Ranga Ram Chary, Gabriel Brammer, Sune Toft
Figure caption: Color vs. magnitude diagram in (B − I) vs. I-band absolute luminosity (in the Vega system). The brown and gray points correspond to the globular clusters around BCGs NGC 7720 and ESO444-G046 in the A2634 and A3558 galaxy clusters, respectively, from Harris et al. (2014). The latter galaxy cluster is 1.7 times more massive than the former but still 1.7 times less massive than SMACS0735. The compact star clusters studied in this work at z = 0.39 are shown as purple circles. They occupy the bright end at relatively blue B − I colors consistent with the more massive of the two local galaxy clusters shown.
Paper: What Are Those Tiny Things? A First Study of Compact Star Clusters in the SMACS0723 Field with JWST
Authors: Andreas L. Faisst, Ranga Ram Chary, Gabriel Brammer, Sune Toft
Figure caption: Individual compact clusters color-coded by their best-fit metallicity (red scale) and age (blue scale). Note that each symbol has two colors assigned (metallicity as edge-color and age as face-color). Light symbols correspond to star clusters with low ages and metallicities, while darker symbols correspond to older and more metal-rich star clusters. The background shows a Gaussian kernel density estimation of the data points for visual guidance of the density of points. The lines show models at different metallicities (color of lines) as a function of age (running from left to right, dots on lines represent ages of 0.5, 1, 4, and 9 Gyr).
Paper: What Are Those Tiny Things? A First Study of Compact Star Clusters in the SMACS0723 Field with JWST
Authors: Andreas L. Faisst, Ranga Ram Chary, Gabriel Brammer, Sune Toft
Figure caption: We use the TRACTOR software package to fit point-source profiles to the selected compact star clusters in the highly blended cluster environment. The first column shows the stacked cutouts in each of the NIRCAM band. The second and third columns show the best-fit model and the residual, respectively. The rows show the fits for the six NIRCam filters. The measured total flux values in nJy are indicated. The intensity scale is the same for each row (the residuals are consistent with zero) and all cutouts are 0.″8 in size.
Paper: Interstellar Meteors Are Outliers in Material Strength
Authors: Amir Siraj, Abraham Loeb
Figure caption: Total power released in the IM1 and IM2 fireballs (navy blue and bright blue lines, respectively) as a function of ram pressure ρ v 2. Peak brightness is reached at 194 and 75 MPa, respectively, for the two fireballs. Typical stony and iron meteorite yield strengths 1–5 and 50 MPa, respectively, are indicated for convenience of comparison. Note that 1 TW = 1019 erg s−1, and 1 MPa = 107 dynes cm−2. The IM2 light curve is calibrated based on the total energy released (taking account of a normalization error in the published light curve). There is an early flare in the IM2 light curve indicating some amount of lower-strength material in addition to the clearly central flare corresponding to a metallic composition.
Paper: Interstellar Meteors Are Outliers in Material Strength
Authors: Amir Siraj, Abraham Loeb
Figure caption: Histogram of ram pressure at breakup ρ v 2 for all fireballs in the CNEOS catalog with altitudes and velocities reported at the times of peak brightness. Navy blue and bright blue correspond to IM1 and IM2, respectively, which are ranked first and third in terms of material strength out of all 273 fireballs. The black line indicates the best fit to a Gaussian with mean and standard deviation matching the data μ = 0.47 and σ = 0.65.
Paper: GOALS-JWST: Tracing AGN Feedback on the Star-forming Interstellar Medium in NGC 7469
Authors: Thomas S.-Y. Lai, 劭愉 賴, Lee Armus, Vivian U, Tanio Díaz-Santos, Kirsten L. Larson, Aaron Evans, Matthew A. Malkan, Philip Appleton, Jeff Rich, Francisco Müller-Sánchez, Hanae Inami, Thomas Bohn, Jed McKinney, Luke Finnerty, David R. Law, Sean T. Linden, Anne M. Medling, George C. Privon, Yiqing Song, Sabrina Stierwalt, Paul P. van der Werf, Loreto Barcos-Muñoz, J. D. T. Smith, Aditya Togi, Susanne Aalto, Torsten Böker, Vassilis Charmandaris, Justin Howell, Kazushi Iwasawa, Francisca Kemper, Joseph M. Mazzarella, Eric J. Murphy, Michael J. I. Brown, Christopher C. Hayward, Jason Marshall, David Sanders, Jason Surace
Figure caption: Extractions of the JWST/MIRI spectra in this study. (a) The 6.2 μm polycyclic aromatic hydrocarbon (PAH) map created by applying a local continuum subtraction using the QFitsView tool (Ott 2012). (b) The same map as (a) overlaid with 17 apertures (each with a diameter of 0.″ 8) used to characterize the dust and line emission of the circumnuclear ring and the inner ISM region. Regions R1–R11 cover mostly the circular ring, while regions R1a, R2a/b, R7a/b, and R10a are used to study changes of the ISM properties in the radial direction. In addition, the central black area marks the region for the nucleus extraction. (c) The nucleus spectrum is shown in purple. Other ring extracted spectra are sorted by the 6.2/7.7 PAH ratio in ascending order from bottom to top. The main PAH features (red) and neon lines (blue) used in this study are highlighted together with the silicate absorption (yellow), which is mainly used for constraining the extinction level in spectral decomposition.
Paper: GOALS-JWST: Tracing AGN Feedback on the Star-forming Interstellar Medium in NGC 7469
Authors: Thomas S.-Y. Lai, 劭愉 賴, Lee Armus, Vivian U, Tanio Díaz-Santos, Kirsten L. Larson, Aaron Evans, Matthew A. Malkan, Philip Appleton, Jeff Rich, Francisco Müller-Sánchez, Hanae Inami, Thomas Bohn, Jed McKinney, Luke Finnerty, David R. Law, Sean T. Linden, Anne M. Medling, George C. Privon, Yiqing Song, Sabrina Stierwalt, Paul P. van der Werf, Loreto Barcos-Muñoz, J. D. T. Smith, Aditya Togi, Susanne Aalto, Torsten Böker, Vassilis Charmandaris, Justin Howell, Kazushi Iwasawa, Francisca Kemper, Joseph M. Mazzarella, Eric J. Murphy, Michael J. I. Brown, Christopher C. Hayward, Jason Marshall, David Sanders, Jason Surace
Figure caption: The interband ratios of the three main polycyclic aromatic hydrocarbon (PAH) bands at 6.2, 7.7, and 11.3 μm in the 17 regions extracted from the star-forming ring. The two tracks indicate the theoretical values for neutral and ionized PAHs with corresponding numbers of carbon atoms from Draine et al. (2021a). The star symbol indicates the PAH ratios derived from the total extraction of NGC 7469 in the MIRI MRS (Armus et al. 2022), while the red diamond is the ratio derived from the central nucleus. For comparison, the galaxies in GOALS (Stierwalt et al. 2014) are shown in gray points, along with points showing the 20%–80% range in star-forming galaxies from surveys of ASESS (Lai et al. 2020) and SINGS (Smith et al. 2007). The gray star indicates the measurement of the combined AKARI+Spitzer spectrum of NGC 7469 in ASESS. (inset) The zoom-in of the regions used for radial variation studies. Regions with a and b designations are those close to the nucleus as shown in Figure 1(b). Every region in the inset shows a trend of decreasing PAH 6.2/7.7 ratio when progressively moving toward the center, suggesting an increase of the grain size distribution.
Paper: GOALS-JWST: Tracing AGN Feedback on the Star-forming Interstellar Medium in NGC 7469
Authors: Thomas S.-Y. Lai, 劭愉 賴, Lee Armus, Vivian U, Tanio Díaz-Santos, Kirsten L. Larson, Aaron Evans, Matthew A. Malkan, Philip Appleton, Jeff Rich, Francisco Müller-Sánchez, Hanae Inami, Thomas Bohn, Jed McKinney, Luke Finnerty, David R. Law, Sean T. Linden, Anne M. Medling, George C. Privon, Yiqing Song, Sabrina Stierwalt, Paul P. van der Werf, Loreto Barcos-Muñoz, J. D. T. Smith, Aditya Togi, Susanne Aalto, Torsten Böker, Vassilis Charmandaris, Justin Howell, Kazushi Iwasawa, Francisca Kemper, Joseph M. Mazzarella, Eric J. Murphy, Michael J. I. Brown, Christopher C. Hayward, Jason Marshall, David Sanders, Jason Surace
Figure caption: (a) The correlation between polycyclic aromatic hydrocarbon (PAH) sizes, as indicated by the 6.2/7.7 PAH ratio, and hardness of the radiation fields. Collectively, PAH 6.2/7.7 shows a slight downward trend, suggesting smaller grains are likely being destroyed as the hardness of the radiation field increases. This effect is more pronounced when compared to points along the same radial direction (linked by dashed lines) with different distances to the nucleus. The nuclear point does not appear to follow this downward trend but it has a relatively large uncertainty. (b) H2-to-PAH ratio shows an increasing trend with increasing [Ne III]/[Ne II]. Here the H2 flux represents the sum of the low rotational lines S(1)–S(5), while PAH represents the flux from the 7.7 μm PAH. We find that H2/PAH in the ring are well within the range of normal PDR models (Guillard et al. 2012), suggesting the H2 gas is predominantly heated by young stars. For comparison, the nucleus lies well above the PDR limit, indicative of either AGN heating or shocks in the vicinity of the AGN.
Paper: GOALS-JWST: Tracing AGN Feedback on the Star-forming Interstellar Medium in NGC 7469
Authors: Thomas S.-Y. Lai, 劭愉 賴, Lee Armus, Vivian U, Tanio Díaz-Santos, Kirsten L. Larson, Aaron Evans, Matthew A. Malkan, Philip Appleton, Jeff Rich, Francisco Müller-Sánchez, Hanae Inami, Thomas Bohn, Jed McKinney, Luke Finnerty, David R. Law, Sean T. Linden, Anne M. Medling, George C. Privon, Yiqing Song, Sabrina Stierwalt, Paul P. van der Werf, Loreto Barcos-Muñoz, J. D. T. Smith, Aditya Togi, Susanne Aalto, Torsten Böker, Vassilis Charmandaris, Justin Howell, Kazushi Iwasawa, Francisca Kemper, Joseph M. Mazzarella, Eric J. Murphy, Michael J. I. Brown, Christopher C. Hayward, Jason Marshall, David Sanders, Jason Surace
Figure caption: (a) R1 Spectrum with the full JWST MIRI MRS coverage from 5 to 28 μm. The dashed line indicates the extinction curve used in the CAFE decomposition. The data are shown in black, and the green line represents the total fit. The gray line shows the underlying continuum made of the cool dust (cyan), warm dust (orange), and hot dust component (not shown). The purple lines sitting above the continuum are the polycyclic aromatic hydrocarbon (PAH) features, while the blue lines are the atomic and molecular spectral lines. (b)–(d) The zoomed-in view of the R1, R7, and R7b continuum-subtracted spectra with key diagnostics and their corresponding wavelengths labeled. These three spectra cover the range of PAH variation in this study and are plotted to the peak of 11.3 μm PAH to ease the comparison between different PAH ratios.
Paper: Early Results from GLASS-JWST. VIII. An Extremely Magnified Blue Supergiant Star at Redshift 2.65 in the A2744 Cluster Field
Authors: Wenlei Chen, Patrick L. Kelly, Tommaso Treu, Xin Wang, Guido Roberts-Borsani, Allison Keen, Rogier A. Windhorst, Rui Zhou, Marusa Bradac, Gabriel Brammer, Victoria Strait, Tom J. Broadhurst, Jose M. Diego, Brenda L. Frye, Ashish K. Meena, Adi Zitrin, Massimo Pascale, Marco Castellano, Danilo Marchesini, Takahiro Morishita, Lilan Yang
Figure caption: The left panel shows the color-composite image of the galaxy-cluster A2744 created from the HST ACS-WFC and WFC3-IR cameras and the location of the newly discovered lensed star in an arc at z = 2.65 (Mahler et al. 2018) in the JWST NIRISS imaging. The six panels on the right show the HST and JWST images of the region enclosed by the red dashed lines in the left panel. The three panels in the middle column show the JWST NIRISS images of the transient (green arrows) acquired by the JWST-ERS-1324 program. The top-right and the middle-right panels are coadded HST WFC3-IR F140W and WFC3-IR F160W images of the region, respectively. The bottom-right panel shows the difference image between the convolved JWST NIRISS F150W image and the combined HST template generated from WFC3-IR F140W and WFC3-IR F160W images. The inset in the top-right corner of the left panel shows the HST ACS-WFC F606W imaging of the sky region enclosed by the white dashed lines. Circle A marks the position of the newly detected transient. The green dashed line illustrates the critical curve whose location is inferred from the mirrored images of the arc. Circle B marks the position of the expected counterimage of A, and we detect no transient at that location. Yellow circles labeled 37.1, 37.2, and 37.3 are a set of multiple images listed in Table A1 in Mahler et al. (2018).
Paper: Early Results from GLASS-JWST. VIII. An Extremely Magnified Blue Supergiant Star at Redshift 2.65 in the A2744 Cluster Field
Authors: Wenlei Chen, Patrick L. Kelly, Tommaso Treu, Xin Wang, Guido Roberts-Borsani, Allison Keen, Rogier A. Windhorst, Rui Zhou, Marusa Bradac, Gabriel Brammer, Victoria Strait, Tom J. Broadhurst, Jose M. Diego, Brenda L. Frye, Ashish K. Meena, Adi Zitrin, Massimo Pascale, Marco Castellano, Danilo Marchesini, Takahiro Morishita, Lilan Yang
Figure caption: Stellar atmosphere models and the measured SED of the transient. The left panel shows 7000 K and 12,000 K models with an R(V) = 3.1 extinction law, as well as best-fitting 8500 K and 7700 K temperatures for extinction laws with R(V) = 3.1 and R(V) = 2.73, respectively. The 7000 K and 12,000 K models are consistent with the measurements within ∼1σ–2σ. The red data points are the photometry of the transient measured from the JWST NIRISS F115W, F150W, and F200W imaging. The panel at the right shows models with 5000 K and 18,000 K where we allow the extinction to vary, and these models are in greater tension with the measurements.
Paper: Early Results from GLASS-JWST. VIII. An Extremely Magnified Blue Supergiant Star at Redshift 2.65 in the A2744 Cluster Field
Authors: Wenlei Chen, Patrick L. Kelly, Tommaso Treu, Xin Wang, Guido Roberts-Borsani, Allison Keen, Rogier A. Windhorst, Rui Zhou, Marusa Bradac, Gabriel Brammer, Victoria Strait, Tom J. Broadhurst, Jose M. Diego, Brenda L. Frye, Ashish K. Meena, Adi Zitrin, Massimo Pascale, Marco Castellano, Danilo Marchesini, Takahiro Morishita, Lilan Yang
Figure caption: Magnification maps for published lens models in the vicinity of the transient. The newly discovered transient event in the JWST NIRISS imaging marked by the green circles is close to the critical curve of the galaxy cluster A2744.
Paper: A First Look at the Abundance Pattern—O/H, C/O, and Ne/O—in z  > 7 Galaxies with JWST/NIRSpec
Authors: Karla Z. Arellano-Córdova, Danielle A. Berg, John Chisholm, Pablo Arrabal Haro, Mark Dickinson, Steven L. Finkelstein, Floriane Leclercq, Noah S. J. Rogers, Raymond C. Simons, Evan D. Skillman, Jonathan R. Trump, Jeyhan S. Kartaltepe
Figure caption: Top left: C/O vs. O/H relationship taken from Berg et al. (2019b) for z ∼ 0 and 2 galaxies. The dashed and solid lines represent the relationships of Garnett et al. (1995) and Nicholls et al. (2017). The results for s04590 are shown as a gray star for the o008 visit. Top right: Ne/O vs. O/H relationship for z ∼ 0 low-metallicity dwarf galaxies and H II regions of spiral galaxies. The Ne/O ratios for the z > 7 NIRSpec galaxies are displayed as gray and cyan symbols. The black dashed line indicates the solar Ne/O value (−0.63 ± 0.05; Asplund et al. 2021). Bottom row: Photoionization models of the [Fe III] λ2465/[O II] λ3727 flux (left) and [Fe II] λ4360/Hγ flux (right) vs. metallicity. The value derived for the Fe III] λ2465/[O II] λ3727 ratio is outside the range of the models (bottom left panel).
Paper: A First Look at the Abundance Pattern—O/H, C/O, and Ne/O—in z  > 7 Galaxies with JWST/NIRSpec
Authors: Karla Z. Arellano-Córdova, Danielle A. Berg, John Chisholm, Pablo Arrabal Haro, Mark Dickinson, Steven L. Finkelstein, Floriane Leclercq, Noah S. J. Rogers, Raymond C. Simons, Evan D. Skillman, Jonathan R. Trump, Jeyhan S. Kartaltepe
Figure caption: The JWST/NIRSpec postprocessed rest-frame spectra of s04590, s06355, and s10612. Wavelength ranges highlighting the important nebular emission line detections are shown. The orange and black spectra correspond to the o007 and o008 visits, respectively, for each galaxy. We highlight the detection of essential emission lines, such as C III] λλ1906, 1906, [Ne III] λ3869, Hγ λ4101, Hδ λ4340, [O III] λ4363, Hβ λ4861, and [O III] λ5007, and the tentative detection of [Fe III] λ2465 in s04590. The inset spectra to the right highlight the differences between the original JWST Science Calibration Pipeline spectrum and the postprocessed spectrum (Trump et al. 2022; P. Arrabal Haro et al., in preparation) for the Hγ and [O III] λ4363 spectral features. The orange and black spectra correspond to the two different postprocessed spectra for the same galaxy, labeled as o007 and o008, respectively, and the original o007 reduction is shown in blue. For all three galaxies, the postprocessed spectra show a higher S/N in the emission lines.
Paper: A First Look at the Abundance Pattern—O/H, C/O, and Ne/O—in z  > 7 Galaxies with JWST/NIRSpec
Authors: Karla Z. Arellano-Córdova, Danielle A. Berg, John Chisholm, Pablo Arrabal Haro, Mark Dickinson, Steven L. Finkelstein, Floriane Leclercq, Noah S. J. Rogers, Raymond C. Simons, Evan D. Skillman, Jonathan R. Trump, Jeyhan S. Kartaltepe
Figure caption: Stellar mass vs. gas-phase metallicity (12 + log(O/H)) relationship for star-forming galaxies. The z > 7 galaxies are plotted as stars with stellar masses derived by Carnall et al. (2023). Additional recent metallicity determinations are labeled from Schaerer et al. (2022; triangles), Trump et al. (2022; pentagons), Curti et al. (2023; diamonds), and Rhoads et al. (2022; squares). For the purpose of comparing to local galaxy populations, we plot the UV-bright CLASSY sample (circles and dashed line; Berg et al. 2022).