adsabs/AstroCLIMB huggingface dataset:
Paper: Estimating Galaxy Parameters with Self-organizing Maps and the Effect of Missing Data
Authors: Valentina La Torre, Anna Sajina, Andy D. Goulding, Danilo Marchesini, Rachel Bezanson, Alan N. Pearl, Laerte Sodré
Figure caption: From left to right, z phot, M *, and SFR predicted vs. true in the cases of recovered missing data for the u band (top) and the H band (middle). The procedure for handling missing data is described in Section 4.5. Bottom: predicted vs. true in the case where only HSC-Deep grizY bands are available and the missing bands are not recovered. Red lines as in Figures 6, 7.
Paper: Estimating Galaxy Parameters with Self-organizing Maps and the Effect of Missing Data
Authors: Valentina La Torre, Anna Sajina, Andy D. Goulding, Danilo Marchesini, Rachel Bezanson, Alan N. Pearl, Laerte Sodré
Figure caption: The true simulated vs. SOM-derived parameter values in the ideal case with no photometric errors. These are based on the K  s -limited test data set. The solid red line represents the bisection line; the red dashed lines indicate the boundaries of the outlier. The number of objects is 232,111.
Paper: Estimating Galaxy Parameters with Self-organizing Maps and the Effect of Missing Data
Authors: Valentina La Torre, Anna Sajina, Andy D. Goulding, Danilo Marchesini, Rachel Bezanson, Alan N. Pearl, Laerte Sodré
Figure caption: The log of the normalized likelihood for a test galaxy (hot diamond) with an upper limit for the H band, in the scenario where the SOM is trained with complete deeper data. The rainbow contours represent levels of redshift values, as in Figure 5.
Paper: The Discovery and Follow-up of Four Transiting Short-period Sub-Neptunes Orbiting M Dwarfs
Authors: Yasunori Hori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, Jerome P. de Leon, Hiroyuki Tako Ishikawa, Joel D. Hartman, Giuseppe Morello, Nestor Abreu García, Leticia Álvarez Hernández, Víctor J. S. Béjar, Yéssica Calatayud-Borras, Ilaria Carleo, Gareb Enoc, Emma Esparza-Borges, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Taiki Kagetani, Yugo Kawai, Kiyoe Kawauchi, Tadahiro Kimura, Takanori Kodama, Judith Korth, Nobuhiko Kusakabe, Andrés Laza-Ramos, John H. Livingston, Rafael Luque, Kohei Miyakawa, Mayuko Mori, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Hannu Parviainen, Alberto Peláez-Torres, Marta Puig-Subirà, Manuel Sánchez-Benavente, Paula Sosa-Guillén, Monika Stangret, Yuka Terada, Sara Muñoz Torres, Noriharu Watanabe, Gaspar Á. Bakos, Khalid Barkaoui, Charles Beichman, Zouhair Benkhaldoun, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J.M. Crossfield, Mark E. Everett, Elise Furlan, Mourad Ghachoui, Michaël Gillon, Erica J. Gonzales, Jesus Higuera, Keith Horne, Steve B. Howell, Emmanuël Jehin, Kathryn V. Lester, Michael B. Lund, Rachel Matson, Elisabeth C. Matthews, Francisco J. Pozuelos, Boris S. Safonov, Joshua E. Schlieder, Richard P. Schwarz, Ramotholo Sefako, Gregor Srdoc, Ivan A. Strakhov, Mathilde Timmermans, William C. Waalkes, Carl Ziegler, David Charbonneau, Zahra Essack, Natalia M. Guerrero, Hiroki Harakawa, Christina Hedges, Masato Ishizuka, Jon M. Jenkins, Mihoko Konishi, Takayuki Kotani, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Jun Nishikawa, Masashi Omiya, George R. Ricker, Sara Seager, Takuma Serizawa, Stephanie Striegel, Motohide Tamura, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn
Figure caption: Top left: the HATSouth light curve of TOI-782 plotted against time. The gray points show the unbinned data, while the red squares show the data binned by 1 day. For clarity, we cut out a gap in the data as shown. The light curve shown in this figure has had an EPD detrending applied to it, but not the more aggressive TFA detrending that is typically also applied to HATSouth light curves. Top right: the GLS unnormalized periodogram of the HATSouth light curve of TOI-782 shows a strong peak at a period of P = 64 days. Middle left: the DACF of the HATSouth EPD light curve. The first and second prominent peaks are fitted with parabolas to determine the period. Middle right: same as on the left, but here we show the DACF of the HATsouth TFA light curve. Some shorter-lag variations in the EPD DACF are not present, suggesting that they are likely due to instrumental systematics. Bottom left: the HATSouth EPD light curve phase folded at the detected period. The gray-scale points show the unbinned data, while the red squares show the phase-binned data with a bin size of 0.02. Bottom right: same as on the left, but here we show only the phase-binned data and zoom in to see the detected photometric variation more clearly.
Paper: The Discovery and Follow-up of Four Transiting Short-period Sub-Neptunes Orbiting M Dwarfs
Authors: Yasunori Hori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, Jerome P. de Leon, Hiroyuki Tako Ishikawa, Joel D. Hartman, Giuseppe Morello, Nestor Abreu García, Leticia Álvarez Hernández, Víctor J. S. Béjar, Yéssica Calatayud-Borras, Ilaria Carleo, Gareb Enoc, Emma Esparza-Borges, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Taiki Kagetani, Yugo Kawai, Kiyoe Kawauchi, Tadahiro Kimura, Takanori Kodama, Judith Korth, Nobuhiko Kusakabe, Andrés Laza-Ramos, John H. Livingston, Rafael Luque, Kohei Miyakawa, Mayuko Mori, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Hannu Parviainen, Alberto Peláez-Torres, Marta Puig-Subirà, Manuel Sánchez-Benavente, Paula Sosa-Guillén, Monika Stangret, Yuka Terada, Sara Muñoz Torres, Noriharu Watanabe, Gaspar Á. Bakos, Khalid Barkaoui, Charles Beichman, Zouhair Benkhaldoun, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J.M. Crossfield, Mark E. Everett, Elise Furlan, Mourad Ghachoui, Michaël Gillon, Erica J. Gonzales, Jesus Higuera, Keith Horne, Steve B. Howell, Emmanuël Jehin, Kathryn V. Lester, Michael B. Lund, Rachel Matson, Elisabeth C. Matthews, Francisco J. Pozuelos, Boris S. Safonov, Joshua E. Schlieder, Richard P. Schwarz, Ramotholo Sefako, Gregor Srdoc, Ivan A. Strakhov, Mathilde Timmermans, William C. Waalkes, Carl Ziegler, David Charbonneau, Zahra Essack, Natalia M. Guerrero, Hiroki Harakawa, Christina Hedges, Masato Ishizuka, Jon M. Jenkins, Mihoko Konishi, Takayuki Kotani, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Jun Nishikawa, Masashi Omiya, George R. Ricker, Sara Seager, Takuma Serizawa, Stephanie Striegel, Motohide Tamura, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn
Figure caption: (a) Detrended and phase-folded light curves of TOI-782 b (upper five curves) and their residuals from the best joint-fitting model (lower five curves). The black, blue, green, orange, and red points (from top to bottom in each of the five data sets) indicate 5 minutes binned data from the TESS, g, r, i, and z  s  bands, respectively. Gray lines indicate the best-fit models. The plots are vertically shifted for display. (b) Top: time series of RV data from Subaru/IRD (blue) along with the 1σ, 2σ, and 3σ credible regions calculated from the posteriors of the joint-fitting analysis (from thick to thin orange). Error bars represent the estimated 1σ uncertainties without a jitter term. Middle: residuals of the RV data from the best joint-fitting model. Bottom: same as the top panel, but phase folded with the orbital period of TOI-782 b. Areas from dark to light orange indicate 1, 2, and 3σ credible regions, respectively.
Paper: The Discovery and Follow-up of Four Transiting Short-period Sub-Neptunes Orbiting M Dwarfs
Authors: Yasunori Hori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, Jerome P. de Leon, Hiroyuki Tako Ishikawa, Joel D. Hartman, Giuseppe Morello, Nestor Abreu García, Leticia Álvarez Hernández, Víctor J. S. Béjar, Yéssica Calatayud-Borras, Ilaria Carleo, Gareb Enoc, Emma Esparza-Borges, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Taiki Kagetani, Yugo Kawai, Kiyoe Kawauchi, Tadahiro Kimura, Takanori Kodama, Judith Korth, Nobuhiko Kusakabe, Andrés Laza-Ramos, John H. Livingston, Rafael Luque, Kohei Miyakawa, Mayuko Mori, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Hannu Parviainen, Alberto Peláez-Torres, Marta Puig-Subirà, Manuel Sánchez-Benavente, Paula Sosa-Guillén, Monika Stangret, Yuka Terada, Sara Muñoz Torres, Noriharu Watanabe, Gaspar Á. Bakos, Khalid Barkaoui, Charles Beichman, Zouhair Benkhaldoun, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J.M. Crossfield, Mark E. Everett, Elise Furlan, Mourad Ghachoui, Michaël Gillon, Erica J. Gonzales, Jesus Higuera, Keith Horne, Steve B. Howell, Emmanuël Jehin, Kathryn V. Lester, Michael B. Lund, Rachel Matson, Elisabeth C. Matthews, Francisco J. Pozuelos, Boris S. Safonov, Joshua E. Schlieder, Richard P. Schwarz, Ramotholo Sefako, Gregor Srdoc, Ivan A. Strakhov, Mathilde Timmermans, William C. Waalkes, Carl Ziegler, David Charbonneau, Zahra Essack, Natalia M. Guerrero, Hiroki Harakawa, Christina Hedges, Masato Ishizuka, Jon M. Jenkins, Mihoko Konishi, Takayuki Kotani, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Jun Nishikawa, Masashi Omiya, George R. Ricker, Sara Seager, Takuma Serizawa, Stephanie Striegel, Motohide Tamura, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn
Figure caption: (a) Power spectra for the g- (top) and r-band (bottom) ZTF light curves of TOI-1448. The gray dashed lines indicate FAPs of 0.1, 1, and 10% from top to bottom. Significant, coincident signals, as shown by the orange vertical lines, can be seen at a period of 42.3 days. (b) The ZTF light curves of TOI-1448 in the g band (top) and the r band (bottom) folded with the peak periods. Light dots and dark circles are unbinned and binned data, respectively. Black curves show the best-fit sine function.
Paper: A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. II. The Radius Cliff Formed by Atmospheric Escape
Authors: Anne Dattilo, Natalie M. Batalha
Figure caption: Occurrence-model comparisons for F, G, and K stellar type bins in insolation-radius space. The three models shown are Rogers & Owen (2021) and Gupta & Schlichting (2020), respectively. Note that the contours for the K star occurrence for core-powered mass-loss are truncated at 0.056% for comparison with all other plots.
Paper: A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. II. The Radius Cliff Formed by Atmospheric Escape
Authors: Anne Dattilo, Natalie M. Batalha
Figure caption: FGK occurrence comparisons with synthetic model populations. First row is occurrence in the period-radius plane, from 1 to 100 days and 2–8R ⊕. Second row is occurrence in the insolation-radius plane, from 104 S ⊕to 10 S ⊕.
Paper: The Discovery and Follow-up of Four Transiting Short-period Sub-Neptunes Orbiting M Dwarfs
Authors: Yasunori Hori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, Jerome P. de Leon, Hiroyuki Tako Ishikawa, Joel D. Hartman, Giuseppe Morello, Nestor Abreu García, Leticia Álvarez Hernández, Víctor J. S. Béjar, Yéssica Calatayud-Borras, Ilaria Carleo, Gareb Enoc, Emma Esparza-Borges, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Taiki Kagetani, Yugo Kawai, Kiyoe Kawauchi, Tadahiro Kimura, Takanori Kodama, Judith Korth, Nobuhiko Kusakabe, Andrés Laza-Ramos, John H. Livingston, Rafael Luque, Kohei Miyakawa, Mayuko Mori, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Hannu Parviainen, Alberto Peláez-Torres, Marta Puig-Subirà, Manuel Sánchez-Benavente, Paula Sosa-Guillén, Monika Stangret, Yuka Terada, Sara Muñoz Torres, Noriharu Watanabe, Gaspar Á. Bakos, Khalid Barkaoui, Charles Beichman, Zouhair Benkhaldoun, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J.M. Crossfield, Mark E. Everett, Elise Furlan, Mourad Ghachoui, Michaël Gillon, Erica J. Gonzales, Jesus Higuera, Keith Horne, Steve B. Howell, Emmanuël Jehin, Kathryn V. Lester, Michael B. Lund, Rachel Matson, Elisabeth C. Matthews, Francisco J. Pozuelos, Boris S. Safonov, Joshua E. Schlieder, Richard P. Schwarz, Ramotholo Sefako, Gregor Srdoc, Ivan A. Strakhov, Mathilde Timmermans, William C. Waalkes, Carl Ziegler, David Charbonneau, Zahra Essack, Natalia M. Guerrero, Hiroki Harakawa, Christina Hedges, Masato Ishizuka, Jon M. Jenkins, Mihoko Konishi, Takayuki Kotani, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Jun Nishikawa, Masashi Omiya, George R. Ricker, Sara Seager, Takuma Serizawa, Stephanie Striegel, Motohide Tamura, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn
Figure caption: Same as Figure 3 but for TOI-2120 b. A linear trend in the RV data was injected in the joint analysis of TOI-2120.
Paper: A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. II. The Radius Cliff Formed by Atmospheric Escape
Authors: Anne Dattilo, Natalie M. Batalha
Figure caption: Occurrence-model comparisons for F, G, and K stellar type bins in period-radius space.
Paper: The Discovery and Follow-up of Four Transiting Short-period Sub-Neptunes Orbiting M Dwarfs
Authors: Yasunori Hori, Akihiko Fukui, Teruyuki Hirano, Norio Narita, Jerome P. de Leon, Hiroyuki Tako Ishikawa, Joel D. Hartman, Giuseppe Morello, Nestor Abreu García, Leticia Álvarez Hernández, Víctor J. S. Béjar, Yéssica Calatayud-Borras, Ilaria Carleo, Gareb Enoc, Emma Esparza-Borges, Izuru Fukuda, Daniel Galán, Samuel Geraldía-González, Yuya Hayashi, Masahiro Ikoma, Kai Ikuta, Keisuke Isogai, Taiki Kagetani, Yugo Kawai, Kiyoe Kawauchi, Tadahiro Kimura, Takanori Kodama, Judith Korth, Nobuhiko Kusakabe, Andrés Laza-Ramos, John H. Livingston, Rafael Luque, Kohei Miyakawa, Mayuko Mori, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Hannu Parviainen, Alberto Peláez-Torres, Marta Puig-Subirà, Manuel Sánchez-Benavente, Paula Sosa-Guillén, Monika Stangret, Yuka Terada, Sara Muñoz Torres, Noriharu Watanabe, Gaspar Á. Bakos, Khalid Barkaoui, Charles Beichman, Zouhair Benkhaldoun, Andrew W. Boyle, David R. Ciardi, Catherine A. Clark, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J.M. Crossfield, Mark E. Everett, Elise Furlan, Mourad Ghachoui, Michaël Gillon, Erica J. Gonzales, Jesus Higuera, Keith Horne, Steve B. Howell, Emmanuël Jehin, Kathryn V. Lester, Michael B. Lund, Rachel Matson, Elisabeth C. Matthews, Francisco J. Pozuelos, Boris S. Safonov, Joshua E. Schlieder, Richard P. Schwarz, Ramotholo Sefako, Gregor Srdoc, Ivan A. Strakhov, Mathilde Timmermans, William C. Waalkes, Carl Ziegler, David Charbonneau, Zahra Essack, Natalia M. Guerrero, Hiroki Harakawa, Christina Hedges, Masato Ishizuka, Jon M. Jenkins, Mihoko Konishi, Takayuki Kotani, Tomoyuki Kudo, Takashi Kurokawa, Masayuki Kuzuhara, Jun Nishikawa, Masashi Omiya, George R. Ricker, Sara Seager, Takuma Serizawa, Stephanie Striegel, Motohide Tamura, Akitoshi Ueda, Roland Vanderspek, Sébastien Vievard, Joshua N. Winn
Figure caption: Same as Figure 3 but for TOI-1448 b.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. II. Deep Constraints on Giant Planets and a Planet Candidate Outside of the Spiral Disk Around SAO 206462
Authors: Gabriele Cugno, Jarron Leisenring, Kevin R. Wagner, Camryn Mullin, Ruobing Dong, Thomas Greene, Doug Johnstone, Michael R. Meyer, Schuyler G. Wolff, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Thomas Roellig, George Rieke, Marcia Rieke, John Stansberry, Erick Young
Figure caption: Injected sources in the F410M JWST/NIRCam data at different PAs (reported on top of each column). The top row shows the residuals without injected point source, the second one reports examples of signal with the same flux as CC1, while the third and the fourth rows show higher confidence (5 and 10σ) detections. The color scale is the same for the first three rows, while the limits have been extended for clarity when plotting the fourth row.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. II. Deep Constraints on Giant Planets and a Planet Candidate Outside of the Spiral Disk Around SAO 206462
Authors: Gabriele Cugno, Jarron Leisenring, Kevin R. Wagner, Camryn Mullin, Ruobing Dong, Thomas Greene, Doug Johnstone, Michael R. Meyer, Schuyler G. Wolff, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Thomas Roellig, George Rieke, Marcia Rieke, John Stansberry, Erick Young
Figure caption: Residuals as shown in the left panel of Figure 2, with the extended diagonal noise feature masked for clarity. North points to the top, east to the left.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. II. Deep Constraints on Giant Planets and a Planet Candidate Outside of the Spiral Disk Around SAO 206462
Authors: Gabriele Cugno, Jarron Leisenring, Kevin R. Wagner, Camryn Mullin, Ruobing Dong, Thomas Greene, Doug Johnstone, Michael R. Meyer, Schuyler G. Wolff, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Thomas Roellig, George Rieke, Marcia Rieke, John Stansberry, Erick Young
Figure caption: F410M residuals highlighting the companion candidate to SAO 206462. Left: residuals of the F410M data, similar to Figure 1. In this instance we applied a larger central mask to force the PCA to focus on the region of the image around ∼1.″9. The data reveals a point source in the NW region of the image. North points to the top, east to the left. Center: zoomed-in portion of the image, highlighting the candidate. The negative-positive-negative pattern, indicative of a point source with the JWST two-rolls observing strategy is clearly visible. Right: same portion of the residuals as in the central panel, but the CC1 pattern was removed injecting one single negative PSF in the data, demonstrating the correlation between the negative and the positive components of the signal.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. II. Deep Constraints on Giant Planets and a Planet Candidate Outside of the Spiral Disk Around SAO 206462
Authors: Gabriele Cugno, Jarron Leisenring, Kevin R. Wagner, Camryn Mullin, Ruobing Dong, Thomas Greene, Doug Johnstone, Michael R. Meyer, Schuyler G. Wolff, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Thomas Roellig, George Rieke, Marcia Rieke, John Stansberry, Erick Young
Figure caption: NIRCam 5σ flux sensitivity limits for SAO 206462 as a function of separation. The dashed vertical line represents the size of the scattered light disk observed in our data, while the gray shaded area highlights the area around 120 ± 30 au where Xie et al. (2021) predicted a planet could be located. The green square represents the measured flux for CC1 in the F410M filter detected with a confidence of ∼3.8σ. On the left (right) side of the plot, we marked the flux expected in the SW (LW) filters for a 1, 2 and 5 M J object at ∼12 Myr according to the BEX evolutionary model.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. II. Deep Constraints on Giant Planets and a Planet Candidate Outside of the Spiral Disk Around SAO 206462
Authors: Gabriele Cugno, Jarron Leisenring, Kevin R. Wagner, Camryn Mullin, Ruobing Dong, Thomas Greene, Doug Johnstone, Michael R. Meyer, Schuyler G. Wolff, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Thomas Roellig, George Rieke, Marcia Rieke, John Stansberry, Erick Young
Figure caption: Mass and temperature limits of SAO 206462 as a function of separation obtained from the 5σ flux limits. The dashed vertical line represents the size of spirals in scattered light and the shaded area highlights the predicted planet location from Xie et al. (2021). Left: mass upper limit when using the BEX cooling curve for the age of the system. The uncertainties, represented by the shaded area, include the age uncertainties of the system (6–16 Myr). The estimated mass of CC1 is showed as a black square. At ∼120 au, the NIRCam data exclude planets with masses ≳2.2 M J. Right: effective temperature 5σ upper limits when assuming protoplanets emit as blackbodies with radii 1, 2, and 3 R J.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. II. Deep Constraints on Giant Planets and a Planet Candidate Outside of the Spiral Disk Around SAO 206462
Authors: Gabriele Cugno, Jarron Leisenring, Kevin R. Wagner, Camryn Mullin, Ruobing Dong, Thomas Greene, Doug Johnstone, Michael R. Meyer, Schuyler G. Wolff, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Thomas Roellig, George Rieke, Marcia Rieke, John Stansberry, Erick Young
Figure caption: Mass accretion rate upper limits as a function of the extinction affecting the lines for planets with masses 1, 5 and 10 M J. Different colors represent different emission lines and different line styles indicate different planetary masses.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. II. Deep Constraints on Giant Planets and a Planet Candidate Outside of the Spiral Disk Around SAO 206462
Authors: Gabriele Cugno, Jarron Leisenring, Kevin R. Wagner, Camryn Mullin, Ruobing Dong, Thomas Greene, Doug Johnstone, Michael R. Meyer, Schuyler G. Wolff, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Thomas Roellig, George Rieke, Marcia Rieke, John Stansberry, Erick Young
Figure caption: SAO 206462 residuals in the four filters observed with our program. The central masks have radii of 0.″3 in F187N, F200W and F405N, and 0.″8 in F410M. In all images North points to the top, East to the left and the field of view is the same. The color scale has been adapted based on the strength of the disk signal.
Paper: JWST/NIRCam Imaging of Young Stellar Objects. II. Deep Constraints on Giant Planets and a Planet Candidate Outside of the Spiral Disk Around SAO 206462
Authors: Gabriele Cugno, Jarron Leisenring, Kevin R. Wagner, Camryn Mullin, Ruobing Dong, Thomas Greene, Doug Johnstone, Michael R. Meyer, Schuyler G. Wolff, Charles Beichman, Martha Boyer, Scott Horner, Klaus Hodapp, Doug Kelly, Don McCarthy, Thomas Roellig, George Rieke, Marcia Rieke, John Stansberry, Erick Young
Figure caption: Color–magnitude diagram of CC1 and the galaxy population from the JAGUAR mock catalog (Williams et al. 2018). Black lines represent the contours including 50%, 80%, 90%, and 95% of the galaxies in the catalog. CC1 is located at the edge of the galaxy population due to its very red colors.