adsabs/AstroCLIMB huggingface dataset:
Paper: Time Dependence of 50–250 MeV Galactic Cosmic-Ray Protons between Solar Cycles 24 and 25, Measured by the High-energy Particle Detector on board the CSES-01 Satellite
Authors: M. Martucci, R. Ammendola, D. Badoni, S. Bartocci, R. Battiston, S. Beolè, W. J. Burger, D. Campana, G. Castellini, P. Cipollone, S. Coli, L. Conti, A. Contin, M. Cristoforetti, G. D'Angelo, C. De Donato, C. De Santis, A. Di Luca, F. M. Follega, G. Gebbia, R. Iuppa, A. Lega, M. Lolli, N. Marcelli, G. Masciantonio, M. Mergè, M. Mese, C. Neubüser, F. Nozzoli, A. Oliva, G. Osteria, L. Pacini, F. Palma, F. Palmonari, B. Panico, A. Parmentier, S. Perciballi, F. Perfetto, P. Picozza, M. Pozzato, G. M. Rebustini, E. Ricci, M. Ricci, S. B. Ricciarini, U. Savino, Z. Sahnoun, V. Scotti, A. Sotgiu, R. Sparvoli, P. Ubertini, V. Vilona, V. Vitale, S. Zoffoli, P. Zuccon, O. P. M. Aslam, M. D. Ngobeni, M. S. Potgieter
Figure caption: Proton and electrons+positrons signal on plane P 1 as a function of the total energy deposited inside the calorimeter (TOWER+LYSO). To better visualize the separation in the plot, only vertical particles have been selected. The blue curves identify the selection employed to discriminate between protons and other populations.
Paper: Time Dependence of 50–250 MeV Galactic Cosmic-Ray Protons between Solar Cycles 24 and 25, Measured by the High-energy Particle Detector on board the CSES-01 Satellite
Authors: M. Martucci, R. Ammendola, D. Badoni, S. Bartocci, R. Battiston, S. Beolè, W. J. Burger, D. Campana, G. Castellini, P. Cipollone, S. Coli, L. Conti, A. Contin, M. Cristoforetti, G. D'Angelo, C. De Donato, C. De Santis, A. Di Luca, F. M. Follega, G. Gebbia, R. Iuppa, A. Lega, M. Lolli, N. Marcelli, G. Masciantonio, M. Mergè, M. Mese, C. Neubüser, F. Nozzoli, A. Oliva, G. Osteria, L. Pacini, F. Palma, F. Palmonari, B. Panico, A. Parmentier, S. Perciballi, F. Perfetto, P. Picozza, M. Pozzato, G. M. Rebustini, E. Ricci, M. Ricci, S. B. Ricciarini, U. Savino, Z. Sahnoun, V. Scotti, A. Sotgiu, R. Sparvoli, P. Ubertini, V. Vilona, V. Vitale, S. Zoffoli, P. Zuccon, O. P. M. Aslam, M. D. Ngobeni, M. S. Potgieter
Figure caption: Computed proton fluxes as a function of kinetic energy for CR 2207 (purple solid line) and CR 2252 (blue solid line) at the Earth are shown together with the corresponding measured fluxes from HEPD-01 (circles).
Paper: First Look at z > 1 Bars in the Rest-frame Near-infrared with JWST Early CEERS Imaging
Authors: Yuchen Guo, Shardha Jogee, Steven L. Finkelstein, Zilei Chen, Eden Wise, Micaela B. Bagley, Guillermo Barro, Stijn Wuyts, Dale D. Kocevski, Jeyhan S. Kartaltepe, Elizabeth J. McGrath, Henry C. Ferguson, Bahram Mobasher, Mauro Giavalisco, Ray A. Lucas, Jorge A. Zavala, Jennifer M. Lotz, Norman A. Grogin, Marc Huertas-Company, Jesús Vega-Ferrero, Nimish P. Hathi, Pablo Arrabal Haro, Mark Dickinson, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, L. Y. Aaron Yung, Bren E. Backhaus, Eric F. Bell, Antonello Calabrò, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Luca Costantin, Darren Croton, Kelcey Davis, Avishai Dekel, Maximilien Franco, Jonathan P. Gardner, Benne W. Holwerda, Taylor A. Hutchison, Viraj Pandya, Pablo G. Pérez-González, Swara Ravindranath, Caitlin Rose, Jonathan R. Trump, Alexander de la Vega, Weichen Wang
Figure caption: Ellipse fits to the JWST NIRCam F444W image of three example barred galaxies (EGS-30836, EGS-24154, and EGS-12823). The left panel for each galaxy shows the F444W image alone (top) and then with the ellipse fits superposed (bottom). Although nearby sources may appear in the images, they are masked during the ellipse fitting. The blue circle at the bottom right of each image represents the PSF FWHM (0.″16 corresponding to ∼1.3 kpc at z ∼ 1–3), and the horizontal bar shows a 0.″5 scale for reference. The size of each image is adjusted with respect to the size of the source, and ranges from 3.″0 × 3.″0 to 3.″9 × 3.″9. The right panel for each galaxy shows the radial profiles of surface brightness (μ), ellipticity (e), and position angle (PA) versus semimajor axis a derived from the ellipse fits. See Section 4.1 for details. PA goes from 0° to −90° clockwise (from N to W) and goes from 0° to 90° counterclockwise (from N to E). The vertical dashed line represents the F444W PSF (0.″16).
Paper: First Look at z > 1 Bars in the Rest-frame Near-infrared with JWST Early CEERS Imaging
Authors: Yuchen Guo, Shardha Jogee, Steven L. Finkelstein, Zilei Chen, Eden Wise, Micaela B. Bagley, Guillermo Barro, Stijn Wuyts, Dale D. Kocevski, Jeyhan S. Kartaltepe, Elizabeth J. McGrath, Henry C. Ferguson, Bahram Mobasher, Mauro Giavalisco, Ray A. Lucas, Jorge A. Zavala, Jennifer M. Lotz, Norman A. Grogin, Marc Huertas-Company, Jesús Vega-Ferrero, Nimish P. Hathi, Pablo Arrabal Haro, Mark Dickinson, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, L. Y. Aaron Yung, Bren E. Backhaus, Eric F. Bell, Antonello Calabrò, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Luca Costantin, Darren Croton, Kelcey Davis, Avishai Dekel, Maximilien Franco, Jonathan P. Gardner, Benne W. Holwerda, Taylor A. Hutchison, Viraj Pandya, Pablo G. Pérez-González, Swara Ravindranath, Caitlin Rose, Jonathan R. Trump, Alexander de la Vega, Weichen Wang
Figure caption: Montage of JWST F444W images showing the rest-frame NIR morphology of the six example barred galaxies presented in this Letter. The bars were identified by applying quantitative criteria to ellipse fits as outlined in Section 4. The labels in the top left of each figure show the CANDELS ID and redshift of each galaxy. The galaxies have spectroscopic redshifts of 1.116, 1.174, 1.217, 1.543, 2.136, and 2.312, and the last two cases represent the highest-redshift bars quantitatively identified and characterized to date. The blue circle at the bottom right of each image represents the point-spread function (PSF) FWHM (0.″16 corresponding to ∼1.3 kpc at z ∼ 2), and the horizontal bar shows a 0.″5 scale for reference. All images are 3.″0 × 3.″0 in size.
Paper: First Look at z > 1 Bars in the Rest-frame Near-infrared with JWST Early CEERS Imaging
Authors: Yuchen Guo, Shardha Jogee, Steven L. Finkelstein, Zilei Chen, Eden Wise, Micaela B. Bagley, Guillermo Barro, Stijn Wuyts, Dale D. Kocevski, Jeyhan S. Kartaltepe, Elizabeth J. McGrath, Henry C. Ferguson, Bahram Mobasher, Mauro Giavalisco, Ray A. Lucas, Jorge A. Zavala, Jennifer M. Lotz, Norman A. Grogin, Marc Huertas-Company, Jesús Vega-Ferrero, Nimish P. Hathi, Pablo Arrabal Haro, Mark Dickinson, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, L. Y. Aaron Yung, Bren E. Backhaus, Eric F. Bell, Antonello Calabrò, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Luca Costantin, Darren Croton, Kelcey Davis, Avishai Dekel, Maximilien Franco, Jonathan P. Gardner, Benne W. Holwerda, Taylor A. Hutchison, Viraj Pandya, Pablo G. Pérez-González, Swara Ravindranath, Caitlin Rose, Jonathan R. Trump, Alexander de la Vega, Weichen Wang
Figure caption: Ellipse fits to the JWST NIRCam F444W image of an unbarred face-on disk galaxy (EGS-17029) and an inclined disk galaxy (EGS-22525). The left panel for each galaxy shows the F444W image alone (top) and then with the ellipse fits superposed (bottom). The blue circle at the bottom right of each image represents the PSF FWHM (0.″16 corresponding to ∼1.3 kpc at z ∼ 1–3), and the horizontal bar shows a 0.″5 scale for reference. The size of each image is adjusted with respect to the size of the source, and ranges from 4.″5 × 4.″5 to 3.″0 × 3.″0. The right panel for each galaxy shows the radial profiles of surface brightness (μ), ellipticity (e), and position angle (PA) versus semimajor axis a derived from the ellipse fits. The vertical dashed line represents the F444W PSF (0.″16). The profiles do not show the characteristic signatures that meet our bar criteria in Section 4.1.
Paper: First Look at z > 1 Bars in the Rest-frame Near-infrared with JWST Early CEERS Imaging
Authors: Yuchen Guo, Shardha Jogee, Steven L. Finkelstein, Zilei Chen, Eden Wise, Micaela B. Bagley, Guillermo Barro, Stijn Wuyts, Dale D. Kocevski, Jeyhan S. Kartaltepe, Elizabeth J. McGrath, Henry C. Ferguson, Bahram Mobasher, Mauro Giavalisco, Ray A. Lucas, Jorge A. Zavala, Jennifer M. Lotz, Norman A. Grogin, Marc Huertas-Company, Jesús Vega-Ferrero, Nimish P. Hathi, Pablo Arrabal Haro, Mark Dickinson, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, L. Y. Aaron Yung, Bren E. Backhaus, Eric F. Bell, Antonello Calabrò, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Luca Costantin, Darren Croton, Kelcey Davis, Avishai Dekel, Maximilien Franco, Jonathan P. Gardner, Benne W. Holwerda, Taylor A. Hutchison, Viraj Pandya, Pablo G. Pérez-González, Swara Ravindranath, Caitlin Rose, Jonathan R. Trump, Alexander de la Vega, Weichen Wang
Figure caption: Same as Figure 2, but for three other example barred galaxies (EGS-26831, EGS-23205, and EGS-24268). See Section 4 for details.
Paper: First Look at z > 1 Bars in the Rest-frame Near-infrared with JWST Early CEERS Imaging
Authors: Yuchen Guo, Shardha Jogee, Steven L. Finkelstein, Zilei Chen, Eden Wise, Micaela B. Bagley, Guillermo Barro, Stijn Wuyts, Dale D. Kocevski, Jeyhan S. Kartaltepe, Elizabeth J. McGrath, Henry C. Ferguson, Bahram Mobasher, Mauro Giavalisco, Ray A. Lucas, Jorge A. Zavala, Jennifer M. Lotz, Norman A. Grogin, Marc Huertas-Company, Jesús Vega-Ferrero, Nimish P. Hathi, Pablo Arrabal Haro, Mark Dickinson, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, L. Y. Aaron Yung, Bren E. Backhaus, Eric F. Bell, Antonello Calabrò, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Luca Costantin, Darren Croton, Kelcey Davis, Avishai Dekel, Maximilien Franco, Jonathan P. Gardner, Benne W. Holwerda, Taylor A. Hutchison, Viraj Pandya, Pablo G. Pérez-González, Swara Ravindranath, Caitlin Rose, Jonathan R. Trump, Alexander de la Vega, Weichen Wang
Figure caption: Effects of bandpass shift and PSF for an example barred galaxy (EGS-23205) at redshift z ∼ 2.136 in our sample. From left to right, we show the HST WFC3 F160W and JWST NIRCam F115W, F150W, F277W, and F444W images. The blue circle at the bottom right of each image represents the point-spread function (PSF) FWHM of each band (0.″18, 0.″07, 0.″07, 0.″13, and 0.″16, respectively) and the horizontal bar shows a 0.″5 scale for reference. All images are 3.″0 × 3.″0 in size. The underlying stellar mass distribution and galactic components, such as the stellar bar, are better traced by the high-resolution rest-frame NIR image revealed by the JWST F444W data than by the rest-frame UV light shown in the JWST F115W images. It is also striking that although the HST F160W and JWST F444W images have a similar PSF (0.″18 and 0.″16, respectively), the bar is more evident in the JWST image due to the longer rest-frame wavelength light the latter is tracing. Signs of the bar are also visible in the high-resolution rest-frame red optical image traced by the JWST F227W data, but are much less evident in the rest-frame blue optical light traced by the JWST F150W image. In all images, N is up, and E is left.
Paper: The PHANGS–JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular Resolution in Nearby GalaxieS
Authors: Janice C. Lee, Karin M. Sandstrom, Adam K. Leroy, David A. Thilker, Eva Schinnerer, Erik Rosolowsky, Kirsten L. Larson, Oleg V. Egorov, Thomas G. Williams, Judy Schmidt, Eric Emsellem, Gagandeep S. Anand, Ashley T. Barnes, Francesco Belfiore, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Jakob den Brok, Yixian Cao, Rupali Chandar, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Enrico Congiu, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Kiana F. Henny, Jonathan D. Henshaw, Nils Hoyer, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Hwihyun Kim, Ralf S. Klessen, Eric W. Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Jing Li, Daizhong Liu, Laura A. Lopez, Daniel Maschmann, Ness Mayker Chen, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Nadine Neumayer, Hsi-An Pan, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Francesca Pinna, M. Jimena Rodríguez, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Rowan J. Smith, Mattia C. Sormani, Fabian Scheuermann, Sophia K. Stuber, Jessica Sutter, Jiayi Sun, 嘉懿 孙, Yu-Hsuan Teng, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore, Alessandro Razza
Figure caption: Top: model SEDs of dust-enshrouded young star clusters with filter coverage of the PHANGS–HST and JWST Treasury programs. Models are of a solar metallicity 104 M ⊙ young star cluster at d = 10 Mpc with varying ages and levels of extinction generated with CIGALE (Boquien et al. 2019; Turner et al. 2021). Colored bands show the eight JWST NIRCAM and MIRI filters, spanning from 2 to 21 μm, selected to probe stellar photospheric emission, PAH features, and the dust continuum. The five UV-visible filters used by PHANGS–HST (Lee et al. 2022) appear in gray. Bottom: normalized throughput for each of the eight filters used in the PHANGS–JWST survey. For comparison, the four Spitzer IRAC filters and MIPS 24 μm filter are also shown. A model dust SED is overplotted to illustrate the features probed by each filter. The three PAH features targeted by our survey are marked.
Paper: The PHANGS–JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular Resolution in Nearby GalaxieS
Authors: Janice C. Lee, Karin M. Sandstrom, Adam K. Leroy, David A. Thilker, Eva Schinnerer, Erik Rosolowsky, Kirsten L. Larson, Oleg V. Egorov, Thomas G. Williams, Judy Schmidt, Eric Emsellem, Gagandeep S. Anand, Ashley T. Barnes, Francesco Belfiore, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Jakob den Brok, Yixian Cao, Rupali Chandar, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Enrico Congiu, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Kiana F. Henny, Jonathan D. Henshaw, Nils Hoyer, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Hwihyun Kim, Ralf S. Klessen, Eric W. Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Jing Li, Daizhong Liu, Laura A. Lopez, Daniel Maschmann, Ness Mayker Chen, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Nadine Neumayer, Hsi-An Pan, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Francesca Pinna, M. Jimena Rodríguez, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Rowan J. Smith, Mattia C. Sormani, Fabian Scheuermann, Sophia K. Stuber, Jessica Sutter, Jiayi Sun, 嘉懿 孙, Yu-Hsuan Teng, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore, Alessandro Razza
Figure caption: Composite gri+Hα+CO images for the 19 galaxies in the PHANGS–JWST Treasury program. The gri+Hα images are constructed from VLT-MUSE full-field spectral mapping (Emsellem et al. 2022), with Hα line emission in red, and combined with ALMA CO(2–1) (Leroy et al. 2021) maps, with CO(2–1) flux in blue. The JWST NIRCam and MIRI footprints have been defined to overlap existing MUSE, ALMA, and HST data. Footprints shown with dashed lines represent observations that had not been executed at time of writing (2022 October) and may rotate slightly due to the range of allowed orient angles specified for the target. The JWST sample spans a factor of ∼50 in stellar mass and SFR and a factor of ∼100 in CO surface density (Table 2). It includes galaxies with prominent dust lanes; a full range of stellar bar, bulge, spiral arm morphologies; and nuclear starburst and AGN activity.
Paper: The PHANGS–JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular Resolution in Nearby GalaxieS
Authors: Janice C. Lee, Karin M. Sandstrom, Adam K. Leroy, David A. Thilker, Eva Schinnerer, Erik Rosolowsky, Kirsten L. Larson, Oleg V. Egorov, Thomas G. Williams, Judy Schmidt, Eric Emsellem, Gagandeep S. Anand, Ashley T. Barnes, Francesco Belfiore, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Jakob den Brok, Yixian Cao, Rupali Chandar, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Enrico Congiu, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Kiana F. Henny, Jonathan D. Henshaw, Nils Hoyer, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Hwihyun Kim, Ralf S. Klessen, Eric W. Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Jing Li, Daizhong Liu, Laura A. Lopez, Daniel Maschmann, Ness Mayker Chen, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Nadine Neumayer, Hsi-An Pan, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Francesca Pinna, M. Jimena Rodríguez, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Rowan J. Smith, Mattia C. Sormani, Fabian Scheuermann, Sophia K. Stuber, Jessica Sutter, Jiayi Sun, 嘉懿 孙, Yu-Hsuan Teng, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore, Alessandro Razza
Figure caption: Left: original calibrated image, presented with a strong intensity transfer function to highlight stripes due to 1/f noise. Middle: PCA noise model, with the displayed intensity range now centered on zero and the intensity scale boosted by a factor of 5 compared to the original image. Right: final destriped data.
Paper: The PHANGS–JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular Resolution in Nearby GalaxieS
Authors: Janice C. Lee, Karin M. Sandstrom, Adam K. Leroy, David A. Thilker, Eva Schinnerer, Erik Rosolowsky, Kirsten L. Larson, Oleg V. Egorov, Thomas G. Williams, Judy Schmidt, Eric Emsellem, Gagandeep S. Anand, Ashley T. Barnes, Francesco Belfiore, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Jakob den Brok, Yixian Cao, Rupali Chandar, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Enrico Congiu, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Kiana F. Henny, Jonathan D. Henshaw, Nils Hoyer, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Hwihyun Kim, Ralf S. Klessen, Eric W. Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Jing Li, Daizhong Liu, Laura A. Lopez, Daniel Maschmann, Ness Mayker Chen, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Nadine Neumayer, Hsi-An Pan, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Francesca Pinna, M. Jimena Rodríguez, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Rowan J. Smith, Mattia C. Sormani, Fabian Scheuermann, Sophia K. Stuber, Jessica Sutter, Jiayi Sun, 嘉懿 孙, Yu-Hsuan Teng, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore, Alessandro Razza
Figure caption: New PHANGS–JWST imaging for NCG 628 (right panels) compared with data previously taken with Spitzer (left panels), illustrating the order-of-magnitude gains in resolution and sensitivity. Comparisons at three different wavelengths are shown. Top panels: Spitzer IRAC 3.6 μm (channel 1) vs. JWST NIRCam F335M. Middle panels: Spitzer IRAC 8 μm (channel 4) vs. JWST MIRI F770W. Bottom panels: Spitzer MIPS 24 μm vs. JWST MIRI F2100W. The Spitzer IRAC and MIPS data are taken from the SINGS program (Kennicutt et al. 2003; Dale et al. 2005). The JWST image is formed from a mosaic of two pointings with NIRCam and three pointings with MIRI.
Paper: The PHANGS–JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular Resolution in Nearby GalaxieS
Authors: Janice C. Lee, Karin M. Sandstrom, Adam K. Leroy, David A. Thilker, Eva Schinnerer, Erik Rosolowsky, Kirsten L. Larson, Oleg V. Egorov, Thomas G. Williams, Judy Schmidt, Eric Emsellem, Gagandeep S. Anand, Ashley T. Barnes, Francesco Belfiore, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Alberto D. Bolatto, Médéric Boquien, Jakob den Brok, Yixian Cao, Rupali Chandar, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Enrico Congiu, Daniel A. Dale, Sinan Deger, Cosima Eibensteiner, Christopher M. Faesi, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Hamid Hassani, Kiana F. Henny, Jonathan D. Henshaw, Nils Hoyer, Annie Hughes, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Hwihyun Kim, Ralf S. Klessen, Eric W. Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Jing Li, Daizhong Liu, Laura A. Lopez, Daniel Maschmann, Ness Mayker Chen, Sharon E. Meidt, Eric J. Murphy, Justus Neumann, Nadine Neumayer, Hsi-An Pan, Ismael Pessa, Jérôme Pety, Miguel Querejeta, Francesca Pinna, M. Jimena Rodríguez, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Rowan J. Smith, Mattia C. Sormani, Fabian Scheuermann, Sophia K. Stuber, Jessica Sutter, Jiayi Sun, 嘉懿 孙, Yu-Hsuan Teng, Robin G. Treß, Antonio Usero, Elizabeth J. Watkins, Bradley C. Whitmore, Alessandro Razza
Figure caption: Comparison of new PHANGS–JWST imaging with data previously taken by Spitzer, now for NGC 7496. Here comparisons at two wavelengths are shown. Left two panels: Spitzer IRAC 3.6 μm (channel 1) vs. JWST NIRCam F335M. Right two panels: Spitzer IRAC 8 μm (channel 4) vs. JWST MIRI F770W.
Paper: PHANGS–JWST First Results: Stellar-feedback-driven Excitation and Dissociation of Molecular Gas in the Starburst Ring of NGC 1365?
Authors: Daizhong Liu, Eva Schinnerer, Yixian Cao, Adam Leroy, Antonio Usero, Erik Rosolowsky, J. M. Diederik Kruijssen, Mélanie Chevance, Simon C. O. Glover, Mattia C. Sormani, Alberto D. Bolatto, Jiayi Sun, Sophia K. Stuber, Yu-Hsuan Teng, Frank Bigiel, Ivana Bešlić, Kathryn Grasha, Jonathan D. Henshaw, Ashley T. Barnes, Jakob S. den Brok, Toshiki Saito, Daniel A. Dale, Elizabeth J. Watkins, Hsi-An Pan, Ralf S. Klessen, Eric Emsellem, Gagandeep S. Anand, Sinan Deger, Oleg V. Egorov, Christopher M. Faesi, Hamid Hassani, Kirsten L. Larson, Janice C. Lee, Laura A. Lopez, Jérôme Pety, Karin Sandstrom, David A. Thilker, Bradley C. Whitmore, Thomas G. Williams
Figure caption: ALMA and JWST images of NGC 1365. Left column (a), (d), (g): native-resolution (0.″3) ALMA CO (2–1) integrated intensity (mom0), line-of-sight velocity (mom1), and velocity dispersion (mom2); see also Schinnerer et al. (2023). Middle column (b), (e), (h): JWST stellar-continuum-dominated NIRCam 2 μm, PAH-dominated MIRI 11.3 μm, and dust-continuum-dominated MIRI 21 μm, all at native resolutions; see also Whitmore et al. (2023). Right column (c), (f), (i): ratio maps in logarithmic scale for R 21 = I CO(2−1)/I CO(1−0), R 42 = I CO(4−3)/I CO(2−1), and R CICO = I [CI] (1−0)/I CO(2−1) at the common resolution of 3.″5 (beam is shown in bottom left). Same contours of I CO(2−1) at 400, 1000, 1500, 2000, and 3000 K km s-1 are shown in all panels. The four regions mentioned in this work are highlighted in panel (a). The cone in panel (d) represents the known ionized gas outflow with a half-opening angle 50°, cone axis inclination 35°, and PA 126° (Hjelm & Lindblad 1996; see also Sandqvist et al. 1995; Lindblad 1999; Venturi et al. 2018; Gao et al. 2021) and the white line indicates the disk kinematic major axis at PA 220° (Jorsater & van Moorsel 1995; Lindblad 1999).