adsabs/AstroCLIMB huggingface dataset:
Paper: JWST Imaging of Earendel, the Extremely Magnified Star at Redshift z = 6.2
Authors: Brian Welch, Dan Coe, Erik Zackrisson, S. E. de Mink, Swara Ravindranath, Jay Anderson, Gabriel Brammer, Larry Bradley, Jinmi Yoon, Patrick Kelly, Jose M. Diego, Rogier Windhorst, Adi Zitrin, Paola Dimauro, Yolanda Jiménez-Teja, Abdurro'uf, Mario Nonino, Ana Acebron, Felipe Andrade-Santos, Roberto J. Avila, Matthew B. Bayliss, Alex Benítez, Tom Broadhurst, Rachana Bhatawdekar, Maruša Bradač, Gabriel B. Caminha, Wenlei Chen, Jan Eldridge, Ebraheem Farag, Michael Florian, Brenda Frye, Seiji Fujimoto, Sebastian Gomez, Alaina Henry, Tiger Y.-Y Hsiao, Taylor A. Hutchison, Bethan L. James, Meridith Joyce, Intae Jung, Gourav Khullar, Rebecca L. Larson, Guillaume Mahler, Nir Mandelker, Stephan McCandliss, Takahiro Morishita, Rosa Newshore, Colin Norman, Kyle O'Connor, Pascal A. Oesch, Masamune Oguri, Masami Ouchi, Marc Postman, Jane R. Rigby, Russell E. Ryan Jr, Soniya Sharma, Keren Sharon, Victoria Strait, Louis-Gregory Strolger, F. X. Timmes, Sune Toft, Michele Trenti, Eros Vanzella, Anton Vikaeus
Figure caption: The SED fits to the observed JWST/NIRCam photometry of Earendel (black circles). (a) Single-star fit using T eff = 15,000 K, SMC metallicity (∼1/7 solar), and a ﹩\mathrm{log}(g)=2.8﹩ stellar atmosphere spectrum from the PoWR OB star grid (Hainich et al. 2019) with moderate mass loss (10−7.58 M ⊙ yr−1 for this particular model) redshifted to z = 6.2 (green spectrum, with green squares indicating the filter-integrated fluxes). Under the assumption of 2μ = 35,000 predicted by the LTM model, this star would need to have ﹩\mathrm{log}({L}_{\mathrm{bol}}/{L}_{\odot })\approx 5.8﹩ to match the observed SED. (b) Double-star fit to Earendel’s JWST/NIRCam photometry using two stars from the Lejeune et al. (1997) stellar atmosphere grid redshifted to z = 6.2. Here the cooler star (red spectrum) has T eff = 9000 K, ﹩\mathrm{log}(g)=1.5﹩, and [M/H] = −1, whereas the hotter star (blue spectrum) has T eff = 34,000 K, ﹩\mathrm{log}(g)=4.0﹩, and [M/H] = −1. For this particular combination of stars and under the assumption that 2μ = 35,000 (LTM) holds for both stars, the colder star would have ﹩\mathrm{log}({L}_{\mathrm{bol}}/{L}_{\odot })\approx 5.3﹩ and the hotter ﹩\mathrm{log}({L}_{\mathrm{bol}}/{L}_{\odot })\approx 5.8﹩. The green spectrum indicates the sum of the flux from the two stars, and the green squares are the corresponding filter-integrated fluxes.
Paper: JWST Imaging of Earendel, the Extremely Magnified Star at Redshift z = 6.2
Authors: Brian Welch, Dan Coe, Erik Zackrisson, S. E. de Mink, Swara Ravindranath, Jay Anderson, Gabriel Brammer, Larry Bradley, Jinmi Yoon, Patrick Kelly, Jose M. Diego, Rogier Windhorst, Adi Zitrin, Paola Dimauro, Yolanda Jiménez-Teja, Abdurro'uf, Mario Nonino, Ana Acebron, Felipe Andrade-Santos, Roberto J. Avila, Matthew B. Bayliss, Alex Benítez, Tom Broadhurst, Rachana Bhatawdekar, Maruša Bradač, Gabriel B. Caminha, Wenlei Chen, Jan Eldridge, Ebraheem Farag, Michael Florian, Brenda Frye, Seiji Fujimoto, Sebastian Gomez, Alaina Henry, Tiger Y.-Y Hsiao, Taylor A. Hutchison, Bethan L. James, Meridith Joyce, Intae Jung, Gourav Khullar, Rebecca L. Larson, Guillaume Mahler, Nir Mandelker, Stephan McCandliss, Takahiro Morishita, Rosa Newshore, Colin Norman, Kyle O'Connor, Pascal A. Oesch, Masamune Oguri, Masami Ouchi, Marc Postman, Jane R. Rigby, Russell E. Ryan Jr, Soniya Sharma, Keren Sharon, Victoria Strait, Louis-Gregory Strolger, F. X. Timmes, Sune Toft, Michele Trenti, Eros Vanzella, Anton Vikaeus
Figure caption: An H-R diagram showing best-fit temperature and luminosity constraints for a single star in gray alongside model stellar evolution tracks by Szecsi et al. (2022) that account for stellar wind mass loss and rotation; see their paper for details. We show metallicities ranging from Z = 0.0088 (top left panel; about 0.7 Z ⊙) to 0.00005 (bottom right panel; about Z SMC/50). The darker gray region covers the range of best-fit magnifications from our five lens models, while the lighter gray region includes the uncertainties on each lens model. The low-luminosity region indicated by the dotted box is allowed within the lens model uncertainties but exceeds the μ = 105 magnification upper limit inferred from microlensing measurements in Welch et al. (2022a). The red and blue dashed lines indicate rough limits for a two-star solution, which would require a hotter star >20,000 K to fit the blue UV slope and a cooler star <13,000 K to fit the observed Balmer break. The large parameter space of two-star solutions coupled with our few photometric data points means we cannot fully constrain these solutions; hence, they are shown as rough limits only.
Paper: JWST Imaging of Earendel, the Extremely Magnified Star at Redshift z = 6.2
Authors: Brian Welch, Dan Coe, Erik Zackrisson, S. E. de Mink, Swara Ravindranath, Jay Anderson, Gabriel Brammer, Larry Bradley, Jinmi Yoon, Patrick Kelly, Jose M. Diego, Rogier Windhorst, Adi Zitrin, Paola Dimauro, Yolanda Jiménez-Teja, Abdurro'uf, Mario Nonino, Ana Acebron, Felipe Andrade-Santos, Roberto J. Avila, Matthew B. Bayliss, Alex Benítez, Tom Broadhurst, Rachana Bhatawdekar, Maruša Bradač, Gabriel B. Caminha, Wenlei Chen, Jan Eldridge, Ebraheem Farag, Michael Florian, Brenda Frye, Seiji Fujimoto, Sebastian Gomez, Alaina Henry, Tiger Y.-Y Hsiao, Taylor A. Hutchison, Bethan L. James, Meridith Joyce, Intae Jung, Gourav Khullar, Rebecca L. Larson, Guillaume Mahler, Nir Mandelker, Stephan McCandliss, Takahiro Morishita, Rosa Newshore, Colin Norman, Kyle O'Connor, Pascal A. Oesch, Masamune Oguri, Masami Ouchi, Marc Postman, Jane R. Rigby, Russell E. Ryan Jr, Soniya Sharma, Keren Sharon, Victoria Strait, Louis-Gregory Strolger, F. X. Timmes, Sune Toft, Michele Trenti, Eros Vanzella, Anton Vikaeus
Figure caption: Image cutouts of Earendel in each JWST filter are shown in the top row in native pixels (SW 0.″031; LW 0.″063). Individual exposure cutouts are fit with a PSF point-source model, and the sums of these four exposure-level models are shown in the middle row. The residuals are also calculated on the level of individual exposures, then summed to produce the bottom row of this figure. The residuals are consistent with noise in each filter, indicating that Earendel is a pointlike source and supporting the interpretation that it is a distant lensed star.
Paper: JWST Imaging of Earendel, the Extremely Magnified Star at Redshift z = 6.2
Authors: Brian Welch, Dan Coe, Erik Zackrisson, S. E. de Mink, Swara Ravindranath, Jay Anderson, Gabriel Brammer, Larry Bradley, Jinmi Yoon, Patrick Kelly, Jose M. Diego, Rogier Windhorst, Adi Zitrin, Paola Dimauro, Yolanda Jiménez-Teja, Abdurro'uf, Mario Nonino, Ana Acebron, Felipe Andrade-Santos, Roberto J. Avila, Matthew B. Bayliss, Alex Benítez, Tom Broadhurst, Rachana Bhatawdekar, Maruša Bradač, Gabriel B. Caminha, Wenlei Chen, Jan Eldridge, Ebraheem Farag, Michael Florian, Brenda Frye, Seiji Fujimoto, Sebastian Gomez, Alaina Henry, Tiger Y.-Y Hsiao, Taylor A. Hutchison, Bethan L. James, Meridith Joyce, Intae Jung, Gourav Khullar, Rebecca L. Larson, Guillaume Mahler, Nir Mandelker, Stephan McCandliss, Takahiro Morishita, Rosa Newshore, Colin Norman, Kyle O'Connor, Pascal A. Oesch, Masamune Oguri, Masami Ouchi, Marc Postman, Jane R. Rigby, Russell E. Ryan Jr, Soniya Sharma, Keren Sharon, Victoria Strait, Louis-Gregory Strolger, F. X. Timmes, Sune Toft, Michele Trenti, Eros Vanzella, Anton Vikaeus
Figure caption: Left: Earendel photometry measurements from 14 analyses by 10 coauthors. Right: photometry renormalized to an average AB mag 27.1 (across filters) along with average SED (across methods) and scatter (error bars) plotted in black.
Paper: JWST Imaging of Earendel, the Extremely Magnified Star at Redshift z = 6.2
Authors: Brian Welch, Dan Coe, Erik Zackrisson, S. E. de Mink, Swara Ravindranath, Jay Anderson, Gabriel Brammer, Larry Bradley, Jinmi Yoon, Patrick Kelly, Jose M. Diego, Rogier Windhorst, Adi Zitrin, Paola Dimauro, Yolanda Jiménez-Teja, Abdurro'uf, Mario Nonino, Ana Acebron, Felipe Andrade-Santos, Roberto J. Avila, Matthew B. Bayliss, Alex Benítez, Tom Broadhurst, Rachana Bhatawdekar, Maruša Bradač, Gabriel B. Caminha, Wenlei Chen, Jan Eldridge, Ebraheem Farag, Michael Florian, Brenda Frye, Seiji Fujimoto, Sebastian Gomez, Alaina Henry, Tiger Y.-Y Hsiao, Taylor A. Hutchison, Bethan L. James, Meridith Joyce, Intae Jung, Gourav Khullar, Rebecca L. Larson, Guillaume Mahler, Nir Mandelker, Stephan McCandliss, Takahiro Morishita, Rosa Newshore, Colin Norman, Kyle O'Connor, Pascal A. Oesch, Masamune Oguri, Masami Ouchi, Marc Postman, Jane R. Rigby, Russell E. Ryan Jr, Soniya Sharma, Keren Sharon, Victoria Strait, Louis-Gregory Strolger, F. X. Timmes, Sune Toft, Michele Trenti, Eros Vanzella, Anton Vikaeus
Figure caption: The HST WFC3/IR F110W fluxes measured over four epochs, spanning 2 yr, for Earendel and two nearby lensed mirror images of a star cluster in the Sunrise Arc. The bottom panel shows fluxes normalized to the geometric mean of the star clusters, which we assume remain at constant flux (not variable and unaffected by microlensing). No significant time variation is observed within the uncertainties.
Paper: A Circumplanetary Dust Ring May Explain the Extreme Spectral Slope of the 10 Myr Young Exoplanet K2-33b
Authors: Kazumasa Ohno, Pa Chia Thao, Andrew W. Mann, Jonathan J. Fortney
Figure caption: Corner plot showing the results of atmosphere-ring retrieval on the transmission spectrum of K2-33b obtained by Thao et al. (2022). The colored regions in the 2D posteriors denote 1σ, 2σ, and 3σ intervals. The right top panel also shows the median transmission spectrum and its 1σ and 2σ uncertainties. The CPDR model succeeds in explaining a factor of 2 variation in the transit depth from optical to near-infrared wavelength. Prominent absorption features across the range from 8 to 30 μm are due to ring particle absorption.
Paper: A Circumplanetary Dust Ring May Explain the Extreme Spectral Slope of the 10 Myr Young Exoplanet K2-33b
Authors: Kazumasa Ohno, Pa Chia Thao, Andrew W. Mann, Jonathan J. Fortney
Figure caption: (Top) Transmission spectra of a Jupiter-mass planet with a CPDR. Different colored lines show the spectra for different ring surface densities. We assume optical properties of SiO2 with a mean particle size and size distribution width of the CPDR as a r = 0.1 μm and σ = 0.5. The ring’s inclination and width are fixed to ϕ = 30 deg and W = 0.5. (Middle) The same as the top panel, but with a different vertical scale. (Bottom) The normal optical depth of the ring. The gray dashed and dotted lines denote the optical depth of 1 and 10−3 to indicate the optically thin regime.
Paper: Detecting the Oscillation and Propagation of the Nascent Dynamic Solar Wind Structure at 2.6 Solar Radii Using Very Long Baseline Interferometry Radio Telescopes
Authors: Maoli Ma, Guifré Molera Calvés, Giuseppe Cimò, Ming Xiong, Peijia Li, Jing Kong, Peijin Zhang, Jiansen He, Lijia Liu, Pradyumna Kummamuru, Chuanpeng Hou, Jasper Edwards, Qinghui Liu, Zhong Chen, Zhanghu Chu, De Wu, Xu Zhao, Zhichao Wang, Songtao Han, Quanquan Zhi, Yingkai Liu, Jonathan Quick, Javier González, Cristina García Miró, Mikhail Kharinov, Andrey Mikhailov, Alexander Neidhardt, Tiziana Venturi, Marco Morsiani, Giuseppe Maccaferri, Bo Xia, Hua Zhang, Longfei Hao
Figure caption: The geometric diagrams of P points in the sky plane on October 9. The distances are marked at UTC 11:00. P Yg,MEX is the P point closest to the Sun from the LOS between MEX and Yg. Other P points are the closest point to the Sun from TIW to the antennas.
Paper: Detecting the Oscillation and Propagation of the Nascent Dynamic Solar Wind Structure at 2.6 Solar Radii Using Very Long Baseline Interferometry Radio Telescopes
Authors: Maoli Ma, Guifré Molera Calvés, Giuseppe Cimò, Ming Xiong, Peijia Li, Jing Kong, Peijin Zhang, Jiansen He, Lijia Liu, Pradyumna Kummamuru, Chuanpeng Hou, Jasper Edwards, Qinghui Liu, Zhong Chen, Zhanghu Chu, De Wu, Xu Zhao, Zhichao Wang, Songtao Han, Quanquan Zhi, Yingkai Liu, Jonathan Quick, Javier González, Cristina García Miró, Mikhail Kharinov, Andrey Mikhailov, Alexander Neidhardt, Tiziana Venturi, Marco Morsiani, Giuseppe Maccaferri, Bo Xia, Hua Zhang, Longfei Hao
Figure caption: The projected radial and latitudinal distance. ((I)–(II)). Radial and latitudinal distance at Ys-Hh, Bd-Hh, Zc-Hh, and Mc-Hh. ((III)–(IV)). Radial and latitudinal distance at Bd-Ys, Zc-Ys, Mc-Ys, Zc-Bd, Mc-Bd, and Mc-Zc.
Paper: A Circumplanetary Dust Ring May Explain the Extreme Spectral Slope of the 10 Myr Young Exoplanet K2-33b
Authors: Kazumasa Ohno, Pa Chia Thao, Andrew W. Mann, Jonathan J. Fortney
Figure caption: Transmission spectra of K2-33b with various mineral compositions of the CPDR compared to a ring-free model (gray line). Importantly, all mineral compositions show prominent absorption features at 10–30 μm, except for FeO.
Paper: A Circumplanetary Dust Ring May Explain the Extreme Spectral Slope of the 10 Myr Young Exoplanet K2-33b
Authors: Kazumasa Ohno, Pa Chia Thao, Andrew W. Mann, Jonathan J. Fortney
Figure caption: Schematic illustration showing how the circumplanetary ring affects the atmospheric transmission spectrum.
Paper: Water and an Escaping Helium Tail Detected in the Hazy and Methane-depleted Atmosphere of HAT-P-18b from JWST NIRISS/SOSS
Authors: Guangwei Fu, Néstor Espinoza, David K. Sing, Joshua D. Lothringer, Leonardo A. Dos Santos, Zafar Rustamkulov, Drake Deming, Eliza M.-R. Kempton, Thaddeus D. Komacek, Heather A. Knutson, Loïc Albert, Klaus Pontoppidan, Kevin Volk, Joseph Filippazzo
Figure caption: The top panel shows the comparison between two independent data reductions and previous observations from the ground (Kirk et al. 2017) and HST/WFC3 (Tsiaras et al. 2018) with no offsets applied. All data show excellent consistency with each other. The middle panel shows the spectrum (Fu version) overplotted with two PHOENIX forward models and two ATMO free chemistry retrieval best-fit models. The higher R = 700 spectrum is in gray and the lower R = 200 spectrum is in black. The retrieval is performed on the R = 700 spectrum. The lack of a clearly identifiable methane feature rules out the solar composition atmosphere. The 100 times solar metallicity and 0.3 C/O forward model provide a decent fit but underpredict the 1.4 μm water feature while overpredicting the 2.3 μm methane feature. The ATMO free chemistry retrieval (with H2O, CO2, CO, and CH4) provides the best-fit model, and an identical retrieval without CH4 gives a comparable fit. The log Bayesian evidence difference of 3.79 corresponds to moderate evidence supporting the detection of methane. The BIC metric slightly favors the retrieval without methane due to one less free fitting parameter. The bottom panel shows the corresponding residuals from the models in the middle panel. All models detect clear water absorption and a hazy atmosphere. The escaping helium part of the spectrum was excluded and modeled separately.
Paper: Water and an Escaping Helium Tail Detected in the Hazy and Methane-depleted Atmosphere of HAT-P-18b from JWST NIRISS/SOSS
Authors: Guangwei Fu, Néstor Espinoza, David K. Sing, Joshua D. Lothringer, Leonardo A. Dos Santos, Zafar Rustamkulov, Drake Deming, Eliza M.-R. Kempton, Thaddeus D. Komacek, Heather A. Knutson, Loïc Albert, Klaus Pontoppidan, Kevin Volk, Joseph Filippazzo
Figure caption: The top panel shows one of the integrations from rateints.fits files; the red lines show the first- and second-order spectra traces. The wavelength-dependent zodiacal light background and three zeroth-order nearby contamination stars are visible in the image. The bottom panel shows the reduced light curve at every pixel bin. Contamination 1 has a minimal effect on the planet spectrum as it is far away from the first order and not extracted in the second order. We detect a time-varying flux level in contamination 2 (∼12% dimming), which is likely caused by an eclipsing binary. Contamination 3 has a spike going across the second-order spectrum, which leads to wavelength-dependent dilution effects. We removed the contaminated parts of the spectrum from sources two and three in the analysis.
Paper: Water and an Escaping Helium Tail Detected in the Hazy and Methane-depleted Atmosphere of HAT-P-18b from JWST NIRISS/SOSS
Authors: Guangwei Fu, Néstor Espinoza, David K. Sing, Joshua D. Lothringer, Leonardo A. Dos Santos, Zafar Rustamkulov, Drake Deming, Eliza M.-R. Kempton, Thaddeus D. Komacek, Heather A. Knutson, Loïc Albert, Klaus Pontoppidan, Kevin Volk, Joseph Filippazzo
Figure caption: We detect escaping helium in HAT-P-18b. The top panel shows the light curve centered at the 1083 nm helium line vs. white light light curve from nearby pixels. The middle panel shows the residual (binned in red) from subtracting the outside helium light curve from the inside helium light curve. The residual clearly shows a deeper transit and a tail after the egress. The vertical gray dashed lines show the first and fourth contact and the horizontal gray dashed line is the zero residual level. The bottom panel is the transmission spectrum of HAT-P-18b at pixel level overplotted with the best-fit p-winds model.
Paper: Water and an Escaping Helium Tail Detected in the Hazy and Methane-depleted Atmosphere of HAT-P-18b from JWST NIRISS/SOSS
Authors: Guangwei Fu, Néstor Espinoza, David K. Sing, Joshua D. Lothringer, Leonardo A. Dos Santos, Zafar Rustamkulov, Drake Deming, Eliza M.-R. Kempton, Thaddeus D. Komacek, Heather A. Knutson, Loïc Albert, Klaus Pontoppidan, Kevin Volk, Joseph Filippazzo
Figure caption: The transit light curve has a clear starspot crossing event starting around midtransit (left panel). The starspot crossing affects the light curve as a function of wavelength with shorter wavelengths being the most affected. We first measure the amplitude of the starspot at each wavelength and then use the PHOENIX stellar models to obtain a best-fit starspot temperature of 3596 ± 31 K (right panel). Assuming other unocculted starspots are at a similar temperature, we then use the stellar flux variability level seen in TESS observations to estimate the dilution effect. We obtain a <20 ppm level dilution effect between 0.6 and 2.8 μm, which is much smaller than the uncertainties in the transmission spectrum.
Paper: Water and an Escaping Helium Tail Detected in the Hazy and Methane-depleted Atmosphere of HAT-P-18b from JWST NIRISS/SOSS
Authors: Guangwei Fu, Néstor Espinoza, David K. Sing, Joshua D. Lothringer, Leonardo A. Dos Santos, Zafar Rustamkulov, Drake Deming, Eliza M.-R. Kempton, Thaddeus D. Komacek, Heather A. Knutson, Loïc Albert, Klaus Pontoppidan, Kevin Volk, Joseph Filippazzo
Figure caption: We explored the effects of vertical mixing and photochemistry using VULCAN (Tsai et al. 2021). The blue line is chemical abundance for H2O, CH4, CO, and CO2 at each pressure level from the PHOENIX forward model assuming equilibrium chemistry and solar composition. The orange, green, and red lines show the abundance with different K zz values. The dashed lines are with photochemistry turned on. The dashed black line and gray shaded regions are the retrieved constraints from ATMO. We see both vertical mixing and photochemistry are effective at removing methane from the atmosphere.
Paper: A 16 hr Transit of Kepler-167 e Observed by the Ground-based Unistellar Telescope Network
Authors: Amaury Perrocheau, Thomas M. Esposito, Paul A. Dalba, Franck Marchis, Arin M. Avsar, Ero Carrera, Michel Douezy, Keiichi Fukui, Ryan Gamurot, Tateki Goto, Bruno Guillet, Petri Kuossari, Jean-Marie Laugier, Pablo Lewin, Margaret A. Loose, Laurent Manganese, Benjamin Mirwald, Hubert Mountz, Marti Mountz, Cory Ostrem, Bruce Parker, Patrick Picard, Michael Primm, Justus Randolph, Jay Runge, Robert Savonnet, Chelsea E. Sharon, Jenny Shih, Masao Shimizu, George Silvis, Georges Simard, Alan Simpson, Thusheeta Sivayogan, Meyer Stein, Denis Trudel, Hiroaki Tsuchiyama, Kevin Wagner, Stefan Will
Figure caption: Transit light curve of Kepler-167 e (top) and residuals (middle) as observed by the Unistellar Network. Relative fluxes from individual data sets are plotted with different colors and symbols. The maximum likelihood model corresponding to the values in Table 1 is the red line and the time axis is defined as the time since that model’s midtransit time. The blue squares are weighted average fluxes of the combined data. The expected transit model and its transit start, middle, and end times are plotted as black broken lines. The bottom panel is the same as the top panel but zooms in on the times the transit occurred and only shows the weighted average fluxes.
Paper: A 16 hr Transit of Kepler-167 e Observed by the Ground-based Unistellar Telescope Network
Authors: Amaury Perrocheau, Thomas M. Esposito, Paul A. Dalba, Franck Marchis, Arin M. Avsar, Ero Carrera, Michel Douezy, Keiichi Fukui, Ryan Gamurot, Tateki Goto, Bruno Guillet, Petri Kuossari, Jean-Marie Laugier, Pablo Lewin, Margaret A. Loose, Laurent Manganese, Benjamin Mirwald, Hubert Mountz, Marti Mountz, Cory Ostrem, Bruce Parker, Patrick Picard, Michael Primm, Justus Randolph, Jay Runge, Robert Savonnet, Chelsea E. Sharon, Jenny Shih, Masao Shimizu, George Silvis, Georges Simard, Alan Simpson, Thusheeta Sivayogan, Meyer Stein, Denis Trudel, Hiroaki Tsuchiyama, Kevin Wagner, Stefan Will
Figure caption: Exoplanet Watch observation of the Kepler-167 e egress. Relative fluxes are the blue dots, with corresponding 1σ error bars. The best-fit transit model from fitting only Unistellar Network data is overlaid in red. This model was not fit to the Exoplanet Watch observations.
Paper: A 16 hr Transit of Kepler-167 e Observed by the Ground-based Unistellar Telescope Network
Authors: Amaury Perrocheau, Thomas M. Esposito, Paul A. Dalba, Franck Marchis, Arin M. Avsar, Ero Carrera, Michel Douezy, Keiichi Fukui, Ryan Gamurot, Tateki Goto, Bruno Guillet, Petri Kuossari, Jean-Marie Laugier, Pablo Lewin, Margaret A. Loose, Laurent Manganese, Benjamin Mirwald, Hubert Mountz, Marti Mountz, Cory Ostrem, Bruce Parker, Patrick Picard, Michael Primm, Justus Randolph, Jay Runge, Robert Savonnet, Chelsea E. Sharon, Jenny Shih, Masao Shimizu, George Silvis, Georges Simard, Alan Simpson, Thusheeta Sivayogan, Meyer Stein, Denis Trudel, Hiroaki Tsuchiyama, Kevin Wagner, Stefan Will
Figure caption: Time frames for eVscope observations of Kepler-167 e. 27 out of the 43 observations (green) were used to construct the final light curve. Vertical lines mark the predicted transit start, middle, and end times.
Paper: The HI Mass Function of Star-forming Galaxies at z ∼ 0.35
Authors: Apurba Bera, Nissim Kanekar, Jayaram N. Chengalur, Jasjeet S. Bagla
Figure caption: The HIMF at z ≈ 0 inferred by combining the local M H I–M  B  relation with the B-band luminosity function, with (A) no assumed scatter in the M H I–M  B  relation, and (B) a scatter of σ = 0.26 dex, equal to that in the local universe (Dénes et al. 2014). In each panel, the blue stars show the HIMF of local galaxies inferred here, while the solid line shows the best-fit Schechter function to the inferred HIMF. The dashed line indicates the HIMF measured from the unbiased ALFALFA survey (Jones et al. 2018). It is clear that the assumption of zero scatter results in a significant underestimate of the number of high-mass galaxies, while the assumption σ = 0.26 dex yields a HIMF that is in good agreement with the directly measured one.
Paper: The HI Mass Function of Star-forming Galaxies at z ∼ 0.35
Authors: Apurba Bera, Nissim Kanekar, Jayaram N. Chengalur, Jasjeet S. Bagla
Figure caption: (A) The HIMF at z ≈ 0.35, inferred by combining our M H I–M  B  relation with the ALHAMBRA B-band luminosity function (López-Sanjuan et al. 2017). The blue stars represent the inferred HIMF of blue galaxies at z ∼ 0.35, while the dashed line shows the ALFALFA HIMF at z ≈ 0 (Jones et al. 2018). (B) The inferred number density of blue star-forming galaxies at z ≈ 0.35 above a given HI mass, as a function of ﹩\mathrm{log}({{\rm{M}}}_{{\rm{H}}\,{\rm\small{I}}})﹩. The dashed curve shows the same quantity in the local universe, from the HIMF of ALFALFA survey (Jones et al. 2018).