adsabs/AstroCLIMB huggingface dataset:
Paper: An Ultrawide Bandwidth Digital Backend System Based on PFB Algorithm for QTT
Authors: Hai-long Zhang, Ya-zhou Zhang, Shao-cong Guo, Xu Du, Na Wang, Jie Wang, Xin-chen Ye, Han Wu, Jian Li, Xin Pei, Qiao Meng
Figure caption: QTT ultrawide bandwidth low-frequency channelization scheme.
Paper: An Ultrawide Bandwidth Digital Backend System Based on PFB Algorithm for QTT
Authors: Hai-long Zhang, Ya-zhou Zhang, Shao-cong Guo, Xu Du, Na Wang, Jie Wang, Xin-chen Ye, Han Wu, Jian Li, Xin Pei, Qiao Meng
Figure caption: QTT ultrawide bandwidth low-frequency pulsar backend data processing flow.
Paper: An Ultrawide Bandwidth Digital Backend System Based on PFB Algorithm for QTT
Authors: Hai-long Zhang, Ya-zhou Zhang, Shao-cong Guo, Xu Du, Na Wang, Jie Wang, Xin-chen Ye, Han Wu, Jian Li, Xin Pei, Qiao Meng
Figure caption: VDIF data frame header information transmitted in the UWL.
Paper: An Ultrawide Bandwidth Digital Backend System Based on PFB Algorithm for QTT
Authors: Hai-long Zhang, Ya-zhou Zhang, Shao-cong Guo, Xu Du, Na Wang, Jie Wang, Xin-chen Ye, Han Wu, Jian Li, Xin Pei, Qiao Meng
Figure caption: Front-end platform Ethernet physical layer module structure.
Paper: An Ultrawide Bandwidth Digital Backend System Based on PFB Algorithm for QTT
Authors: Hai-long Zhang, Ya-zhou Zhang, Shao-cong Guo, Xu Du, Na Wang, Jie Wang, Xin-chen Ye, Han Wu, Jian Li, Xin Pei, Qiao Meng
Figure caption: The 20-point FFT structure.
Paper: An Ultrawide Bandwidth Digital Backend System Based on PFB Algorithm for QTT
Authors: Hai-long Zhang, Ya-zhou Zhang, Shao-cong Guo, Xu Du, Na Wang, Jie Wang, Xin-chen Ye, Han Wu, Jian Li, Xin Pei, Qiao Meng
Figure caption: PFB structure.
Paper: An Ultrawide Bandwidth Digital Backend System Based on PFB Algorithm for QTT
Authors: Hai-long Zhang, Ya-zhou Zhang, Shao-cong Guo, Xu Du, Na Wang, Jie Wang, Xin-chen Ye, Han Wu, Jian Li, Xin Pei, Qiao Meng
Figure caption: Front-end platform high-speed Ethernet transmission module.
Paper: Assessing the Association between the Globular Cluster NGC 4147 and the Sagittarius Dwarf Galaxy
Authors: Ying-Hua Zhang, Jundan Nie, Hao Tian, Chao Liu
Figure caption: Left panel: the CMD fitting of NGC 4147. Black dots represent stars inside the tidal radius of NGC 4147, excluding the innermost center, i.e., ﹩2\buildrel{\,\prime}\over{.} 5\lt {r}_{t}\lt 6\buildrel{\,\prime}\over{.} 6﹩. Typical observational errors are shown from 17 to 22.7 mag with red bars. The result of the best CMD fitting is τ = 11.0 Gyr, Z = 0.0006, and d ⊙ = 18.5 kpc (blue line). Right panel: the background-subtracted Hess diagram for NGC 4147, considered as the final CMD template.
Paper: Assessing the Association between the Globular Cluster NGC 4147 and the Sagittarius Dwarf Galaxy
Authors: Ying-Hua Zhang, Jundan Nie, Hao Tian, Chao Liu
Figure caption: Left panel: the significance distribution of the density centered by the core of the cluster shows the final extratidal structure of NGC 4147. The black dashed circle indicates the tidal radius of NGC 4147. Different colors indicate the significance levels with a black line for 3.0σ. The blue arrow indicates the direction to the Galactic center, the red arrow for the Sgr orbit, and the black one for the NGC 4147 orbit. Right panel: the extinction map of the same region.
Paper: Assessing the Association between the Globular Cluster NGC 4147 and the Sagittarius Dwarf Galaxy
Authors: Ying-Hua Zhang, Jundan Nie, Hao Tian, Chao Liu
Figure caption: Left panel: LFs in three different regions: ﹩2\buildrel{\,\prime}\over{.} 5\lt {r}_{t}\lt 4\buildrel{\,\prime}\over{.} 3﹩, ﹩4\buildrel{\,\prime}\over{.} 3\lt {r}_{t}\lt 6\buildrel{\,\prime}\over{.} 6﹩, and ﹩6\buildrel{\,\prime}\over{.} 6\lt {r}_{t}\lt 9\buildrel{\,\prime}\over{.} 0﹩. The star count is normalized at r = 20.45 mag. Right panel: mass functions of NGC 4147. The error bars are a 1σ Poisson error derived from number counts. The solid lines show the best-fit power laws.
Paper: Assessing the Association between the Globular Cluster NGC 4147 and the Sagittarius Dwarf Galaxy
Authors: Ying-Hua Zhang, Jundan Nie, Hao Tian, Chao Liu
Figure caption: Relationships between the angular momentum along the z-direction Lz vs. total orbital energy E. The gray dots show the distribution of Sgr stream stars, and the cyan dots are the ones near NGC 4147 in space position. The black star represents the Sgr dSph core and the red one NGC 4147. The black circles are the GCs associated with Sgr. The blue dots stand for the high-probability member stars of NGC 4147. The red dashed box denotes the region of concentrated energy–angular momentum within the GSE (collected from D. Massari et al. 2019).
Paper: Assessing the Association between the Globular Cluster NGC 4147 and the Sagittarius Dwarf Galaxy
Authors: Ying-Hua Zhang, Jundan Nie, Hao Tian, Chao Liu
Figure caption: Left panels: the comparison of stars’ position inside and outside the structure of NGC 4147. Middle panels: the comparison of the CMD. Right panels: the comparison of the PM diagram. In all panels, black dots denote stars inside the tidal radius (﹩2\buildrel{\,\prime}\over{.} 5\lt {r}_{t}\lt 6\buildrel{\,\prime}\over{.} 6﹩), red circles denote all stars inside the multiarmed structure (and ﹩{r}_{t}\gt 6\buildrel{\,\prime}\over{.} 6﹩), and blue circles denote comparing stars outside the structure (i.e., region without MF signal).
Paper: Assessing the Association between the Globular Cluster NGC 4147 and the Sagittarius Dwarf Galaxy
Authors: Ying-Hua Zhang, Jundan Nie, Hao Tian, Chao Liu
Figure caption: The background determination for the MF technique. Left panel: The spatial distribution of the four selected background regions. The red cross marks the center of NGC 4147, and the cyan small squares indicate the MF structure regions. Right panel: HESS diagram of the background.
Paper: Assessing the Association between the Globular Cluster NGC 4147 and the Sagittarius Dwarf Galaxy
Authors: Ying-Hua Zhang, Jundan Nie, Hao Tian, Chao Liu
Figure caption: The completeness function for all point sources in our working field. Different colors represent varying distances from the cluster center. The limit magnitudes in the g- and r-band are 23.2 and 22.7 mag, respectively.
Paper: Assessing the Association between the Globular Cluster NGC 4147 and the Sagittarius Dwarf Galaxy
Authors: Ying-Hua Zhang, Jundan Nie, Hao Tian, Chao Liu
Figure caption: The orbits of Sgr stream model particles and NGC 4147. Left panel: the colored dots represent the Pcol (from the LM10 model), while the black line shows the orbit of NGC 4147 in the R.A.–decl. planes. Right panel: in the X–Z planes.
Paper: An Earth-sized Planet on the Verge of Tidal Disruption
Authors: Fei Dai, Andrew W. Howard, Samuel Halverson, Jaume Orell-Miquel, Enric Pallé, Howard Isaacson, Benjamin Fulton, Ellen M. Price, Mykhaylo Plotnykov, Leslie A. Rogers, Diana Valencia, Kimberly Paragas, Michael Greklek-McKeon, Jonathan Gomez Barrientos, Heather A. Knutson, Erik A. Petigura, Lauren M. Weiss, Rena Lee, Casey L. Brinkman, Daniel Huber, Gumundur Stefánsson, Kento Masuda, Steven Giacalone, Cicero X. Lu, Edwin S. Kite, Renyu Hu, Eric Gaidos, Michael Zhang, Ryan A. Rubenzahl, Joshua N. Winn, Te Han, Corey Beard, Rae Holcomb, Aaron Householder, Gregory J. Gilbert, Jack Lubin, J. M. Joel Ong, Alex S. Polanski, Nicholas Saunders, Judah Van Zandt, Samuel W. Yee, Jingwen Zhang, Jon Zink, Bradford Holden, Ashley Baker, Max Brodheim, Ian J. M. Crossfield, William Deich, Jerry Edelstein, Steven R. Gibson, Grant M. Hill, Sharon R Jelinsky, Marc Kassis, Russ R. Laher, Kyle Lanclos, Scott Lilley, Joel N. Payne, Kodi Rider, Paul Robertson, Arpita Roy, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Chris Smith, Adam Vandenberg, Josh Walawender, Sharon X. Wang, Shin-Ywan (Cindy) Wang, Edward Wishnow, Jason T. Wright, Sherry Yeh, José A. Caballero, Juan C. Morales, Felipe Murgas, Evangelos Nagel, Ansgar Reiners, Andreas Schweitzer, Hugo M. Tabernero, Mathias Zechmeister, Alton Spencer, David R. Ciardi, Catherine A. Clark, Michael B. Lund, Douglas A. Caldwell, Karen A. Collins, Richard P. Schwarz, Khalid Barkaoui, Cristilyn Watkins, Avi Shporer, Norio Narita, Akihiko Fukui, Gregor Srdoc, David W. Latham, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek
Figure caption: Top: with an orbital period of 5.7 hr and a semimajor axis (a/R ⋆ = 3.1), TOI-6255 b is close to the tidal disruption limit. K2-137 b (Smith et al. 2018) and KOI-1843.03 have shorter orbital periods. However, the masses of those planets are unknown. Middle: using the equation for the Roche limit P Roche ≈ 12.6 hr × (ρ  p /1 g cm−3)−1/2 from Rappaport et al. (2013), one can compute how far a planet is away from tidal disruption P orb/P Roche. TOI-6255 b stands out as being on the verge of tidal disruption, with P orb/P Roche = 1.13 ± 0.10. The y-axis is how fast the planet would reach the Roche limit due to equilibrium stellar tides (Equation (13); notice the strong dependence on orbital distance). TOI-6255 b may experience the fate of tidal disruption in the next 400 Myr if the tidal quality factor of the star ﹩{Q}_{\star }^{{\prime} }={10}^{7}﹩. The error bar is at least an order of magnitude due to the uncertainty on ﹩{Q}_{\star }^{{\prime} }﹩. Bottom: tidal distortion (the fractional difference between the long axis and the short axis of the ellipsoid) as predicted by tidal Love theory (Equation (4)) with a Love number h 2 = 1. TOI-6255 b is likely the most tidally distorted terrestrial planet discovered so far.
Paper: An Earth-sized Planet on the Verge of Tidal Disruption
Authors: Fei Dai, Andrew W. Howard, Samuel Halverson, Jaume Orell-Miquel, Enric Pallé, Howard Isaacson, Benjamin Fulton, Ellen M. Price, Mykhaylo Plotnykov, Leslie A. Rogers, Diana Valencia, Kimberly Paragas, Michael Greklek-McKeon, Jonathan Gomez Barrientos, Heather A. Knutson, Erik A. Petigura, Lauren M. Weiss, Rena Lee, Casey L. Brinkman, Daniel Huber, Gumundur Stefánsson, Kento Masuda, Steven Giacalone, Cicero X. Lu, Edwin S. Kite, Renyu Hu, Eric Gaidos, Michael Zhang, Ryan A. Rubenzahl, Joshua N. Winn, Te Han, Corey Beard, Rae Holcomb, Aaron Householder, Gregory J. Gilbert, Jack Lubin, J. M. Joel Ong, Alex S. Polanski, Nicholas Saunders, Judah Van Zandt, Samuel W. Yee, Jingwen Zhang, Jon Zink, Bradford Holden, Ashley Baker, Max Brodheim, Ian J. M. Crossfield, William Deich, Jerry Edelstein, Steven R. Gibson, Grant M. Hill, Sharon R Jelinsky, Marc Kassis, Russ R. Laher, Kyle Lanclos, Scott Lilley, Joel N. Payne, Kodi Rider, Paul Robertson, Arpita Roy, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Chris Smith, Adam Vandenberg, Josh Walawender, Sharon X. Wang, Shin-Ywan (Cindy) Wang, Edward Wishnow, Jason T. Wright, Sherry Yeh, José A. Caballero, Juan C. Morales, Felipe Murgas, Evangelos Nagel, Ansgar Reiners, Andreas Schweitzer, Hugo M. Tabernero, Mathias Zechmeister, Alton Spencer, David R. Ciardi, Catherine A. Clark, Michael B. Lund, Douglas A. Caldwell, Karen A. Collins, Richard P. Schwarz, Khalid Barkaoui, Cristilyn Watkins, Avi Shporer, Norio Narita, Akihiko Fukui, Gregor Srdoc, David W. Latham, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek
Figure caption: Precise mass and radius measurements of exoplanets <1.8R ⊕ (from the NASA Exoplanet Archive) and theoretical mass–radius relationships (Zeng et al. 2019). The USP planets (P orb < 1 day, R  p  < 1.8R ⊕; blue points) are so strongly irradiated that they should be bare rocky bodies devoid of H/He envelopes. The existing sample of USP planets is dominated by super-Earths (>2M ⊕). As an ensemble, they cluster around an Earth-like 30% Fe–70% MgSiO3 composition (Dai et al. 2019). TOI-6255 b is in the domain of Earth-sized planets. TOI-6255 b has a CMF of 45% ± 32% (red diamond). If accounting for the tidal distortion with a Love number h 2 = 1, the inferred CMF drops to a CMF of 31% ± 30%, because during transit the shorter two axes of the ellipsoidal planet are visible (brown diamond). See Section 5.2 for details.
Paper: An Earth-sized Planet on the Verge of Tidal Disruption
Authors: Fei Dai, Andrew W. Howard, Samuel Halverson, Jaume Orell-Miquel, Enric Pallé, Howard Isaacson, Benjamin Fulton, Ellen M. Price, Mykhaylo Plotnykov, Leslie A. Rogers, Diana Valencia, Kimberly Paragas, Michael Greklek-McKeon, Jonathan Gomez Barrientos, Heather A. Knutson, Erik A. Petigura, Lauren M. Weiss, Rena Lee, Casey L. Brinkman, Daniel Huber, Gumundur Stefánsson, Kento Masuda, Steven Giacalone, Cicero X. Lu, Edwin S. Kite, Renyu Hu, Eric Gaidos, Michael Zhang, Ryan A. Rubenzahl, Joshua N. Winn, Te Han, Corey Beard, Rae Holcomb, Aaron Householder, Gregory J. Gilbert, Jack Lubin, J. M. Joel Ong, Alex S. Polanski, Nicholas Saunders, Judah Van Zandt, Samuel W. Yee, Jingwen Zhang, Jon Zink, Bradford Holden, Ashley Baker, Max Brodheim, Ian J. M. Crossfield, William Deich, Jerry Edelstein, Steven R. Gibson, Grant M. Hill, Sharon R Jelinsky, Marc Kassis, Russ R. Laher, Kyle Lanclos, Scott Lilley, Joel N. Payne, Kodi Rider, Paul Robertson, Arpita Roy, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Chris Smith, Adam Vandenberg, Josh Walawender, Sharon X. Wang, Shin-Ywan (Cindy) Wang, Edward Wishnow, Jason T. Wright, Sherry Yeh, José A. Caballero, Juan C. Morales, Felipe Murgas, Evangelos Nagel, Ansgar Reiners, Andreas Schweitzer, Hugo M. Tabernero, Mathias Zechmeister, Alton Spencer, David R. Ciardi, Catherine A. Clark, Michael B. Lund, Douglas A. Caldwell, Karen A. Collins, Richard P. Schwarz, Khalid Barkaoui, Cristilyn Watkins, Avi Shporer, Norio Narita, Akihiko Fukui, Gregor Srdoc, David W. Latham, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek
Figure caption: A schematic showing the rotational deformation (top left), tidal distortion (top right), and the combined effect for a synchronously rotating planet (bottom). The host star is located along the x-axis. The orbital motion is against the y-axis direction. The amount of distortion has been exaggerated for visualization. The red, magenta, and blue arrows indicate the long, intermediate, and short semi-axes of the ellipsoid ([R 1, R 2, R 3]). Rotational deformation produces an oblate planet with a bulge at the equator (see Equation (8)). Tidal distortion is along the axis joining the planet and the host star (see Equation (4)).
Paper: An Earth-sized Planet on the Verge of Tidal Disruption
Authors: Fei Dai, Andrew W. Howard, Samuel Halverson, Jaume Orell-Miquel, Enric Pallé, Howard Isaacson, Benjamin Fulton, Ellen M. Price, Mykhaylo Plotnykov, Leslie A. Rogers, Diana Valencia, Kimberly Paragas, Michael Greklek-McKeon, Jonathan Gomez Barrientos, Heather A. Knutson, Erik A. Petigura, Lauren M. Weiss, Rena Lee, Casey L. Brinkman, Daniel Huber, Gumundur Stefánsson, Kento Masuda, Steven Giacalone, Cicero X. Lu, Edwin S. Kite, Renyu Hu, Eric Gaidos, Michael Zhang, Ryan A. Rubenzahl, Joshua N. Winn, Te Han, Corey Beard, Rae Holcomb, Aaron Householder, Gregory J. Gilbert, Jack Lubin, J. M. Joel Ong, Alex S. Polanski, Nicholas Saunders, Judah Van Zandt, Samuel W. Yee, Jingwen Zhang, Jon Zink, Bradford Holden, Ashley Baker, Max Brodheim, Ian J. M. Crossfield, William Deich, Jerry Edelstein, Steven R. Gibson, Grant M. Hill, Sharon R Jelinsky, Marc Kassis, Russ R. Laher, Kyle Lanclos, Scott Lilley, Joel N. Payne, Kodi Rider, Paul Robertson, Arpita Roy, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Chris Smith, Adam Vandenberg, Josh Walawender, Sharon X. Wang, Shin-Ywan (Cindy) Wang, Edward Wishnow, Jason T. Wright, Sherry Yeh, José A. Caballero, Juan C. Morales, Felipe Murgas, Evangelos Nagel, Ansgar Reiners, Andreas Schweitzer, Hugo M. Tabernero, Mathias Zechmeister, Alton Spencer, David R. Ciardi, Catherine A. Clark, Michael B. Lund, Douglas A. Caldwell, Karen A. Collins, Richard P. Schwarz, Khalid Barkaoui, Cristilyn Watkins, Avi Shporer, Norio Narita, Akihiko Fukui, Gregor Srdoc, David W. Latham, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek
Figure caption: Top: the transit of TOI-6255 b as observed by TESS. The black error bars are the phase-folded and binned TESS light curve. The red curve is our best-fit transit model. The blue dotted line also includes the effect of tidal distortion. Middle: the residual flux after removing the best-fit spherical planet model. Bottom: the correction due to tidal distortion amounts to no more than 10 ppm for TOI-6255 b. This is much smaller than the TESS photometric precision and remains unconstrained.
Paper: An Earth-sized Planet on the Verge of Tidal Disruption
Authors: Fei Dai, Andrew W. Howard, Samuel Halverson, Jaume Orell-Miquel, Enric Pallé, Howard Isaacson, Benjamin Fulton, Ellen M. Price, Mykhaylo Plotnykov, Leslie A. Rogers, Diana Valencia, Kimberly Paragas, Michael Greklek-McKeon, Jonathan Gomez Barrientos, Heather A. Knutson, Erik A. Petigura, Lauren M. Weiss, Rena Lee, Casey L. Brinkman, Daniel Huber, Gumundur Stefánsson, Kento Masuda, Steven Giacalone, Cicero X. Lu, Edwin S. Kite, Renyu Hu, Eric Gaidos, Michael Zhang, Ryan A. Rubenzahl, Joshua N. Winn, Te Han, Corey Beard, Rae Holcomb, Aaron Householder, Gregory J. Gilbert, Jack Lubin, J. M. Joel Ong, Alex S. Polanski, Nicholas Saunders, Judah Van Zandt, Samuel W. Yee, Jingwen Zhang, Jon Zink, Bradford Holden, Ashley Baker, Max Brodheim, Ian J. M. Crossfield, William Deich, Jerry Edelstein, Steven R. Gibson, Grant M. Hill, Sharon R Jelinsky, Marc Kassis, Russ R. Laher, Kyle Lanclos, Scott Lilley, Joel N. Payne, Kodi Rider, Paul Robertson, Arpita Roy, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Chris Smith, Adam Vandenberg, Josh Walawender, Sharon X. Wang, Shin-Ywan (Cindy) Wang, Edward Wishnow, Jason T. Wright, Sherry Yeh, José A. Caballero, Juan C. Morales, Felipe Murgas, Evangelos Nagel, Ansgar Reiners, Andreas Schweitzer, Hugo M. Tabernero, Mathias Zechmeister, Alton Spencer, David R. Ciardi, Catherine A. Clark, Michael B. Lund, Douglas A. Caldwell, Karen A. Collins, Richard P. Schwarz, Khalid Barkaoui, Cristilyn Watkins, Avi Shporer, Norio Narita, Akihiko Fukui, Gregor Srdoc, David W. Latham, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek
Figure caption: The RV variation of TOI-6255 b plotted as a function of the orbital phase. Top: the results of our GP model, where long-term stellar activities and instrumental effects have been removed before plotting. Bottom: an alternative model (Floating Chunk Offset; Section 4.4), where observations taken on a single calendar night were given an independent offset (plotted with a different color). These two models give consistent results on the RV semi-amplitude of TOI-6255 b (K = 2.98 ± 0.28 m s−1 vs. K = 2.93 ± 0.38 m s−1).
Paper: An Earth-sized Planet on the Verge of Tidal Disruption
Authors: Fei Dai, Andrew W. Howard, Samuel Halverson, Jaume Orell-Miquel, Enric Pallé, Howard Isaacson, Benjamin Fulton, Ellen M. Price, Mykhaylo Plotnykov, Leslie A. Rogers, Diana Valencia, Kimberly Paragas, Michael Greklek-McKeon, Jonathan Gomez Barrientos, Heather A. Knutson, Erik A. Petigura, Lauren M. Weiss, Rena Lee, Casey L. Brinkman, Daniel Huber, Gumundur Stefánsson, Kento Masuda, Steven Giacalone, Cicero X. Lu, Edwin S. Kite, Renyu Hu, Eric Gaidos, Michael Zhang, Ryan A. Rubenzahl, Joshua N. Winn, Te Han, Corey Beard, Rae Holcomb, Aaron Householder, Gregory J. Gilbert, Jack Lubin, J. M. Joel Ong, Alex S. Polanski, Nicholas Saunders, Judah Van Zandt, Samuel W. Yee, Jingwen Zhang, Jon Zink, Bradford Holden, Ashley Baker, Max Brodheim, Ian J. M. Crossfield, William Deich, Jerry Edelstein, Steven R. Gibson, Grant M. Hill, Sharon R Jelinsky, Marc Kassis, Russ R. Laher, Kyle Lanclos, Scott Lilley, Joel N. Payne, Kodi Rider, Paul Robertson, Arpita Roy, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Chris Smith, Adam Vandenberg, Josh Walawender, Sharon X. Wang, Shin-Ywan (Cindy) Wang, Edward Wishnow, Jason T. Wright, Sherry Yeh, José A. Caballero, Juan C. Morales, Felipe Murgas, Evangelos Nagel, Ansgar Reiners, Andreas Schweitzer, Hugo M. Tabernero, Mathias Zechmeister, Alton Spencer, David R. Ciardi, Catherine A. Clark, Michael B. Lund, Douglas A. Caldwell, Karen A. Collins, Richard P. Schwarz, Khalid Barkaoui, Cristilyn Watkins, Avi Shporer, Norio Narita, Akihiko Fukui, Gregor Srdoc, David W. Latham, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek
Figure caption: RV variations of TOI-6255 b (orange dashed line) measured by KPF (circles) and CARMENES (stars). A GP model (blue dotted line) has been included to remove any stellar activity and instrumental variation on timescales longer than the orbital period of TOI-6255 b. On 2023 November 24, we took a set of 21 continuous exposures of TOI-6255 with KPF (inset). The resultant RVs clearly reveal the 5.7 hr orbit of TOI-6255 b.
Paper: Electron Density Distribution in H II Regions in IC 10
Authors: Fiorella L. Polles, Dario Fadda, William D. Vacca, Nicholas P. Abel, Mélanie Chevance, Christian Fischer, James M. Jackson, Vianney Lebouteiller, Suzanne Madden, Lise Ramambason
Figure caption: Theoretical ratios of [O III] λ88 μm/[O III] λ52 μm toward different regions of IC 10 (Figure 2), determined at the temperature of 9700 K as a function of the electron density n e. The different symbols indicate the observed line-ratio values. Each color and symbol corresponds to one region, and the sizes of the symbol increase as the area considered for the integrated flux ratios increases. The gray area shows the uncertainty due to the temperature’s uncertainty: the range is between 103.89 and 104.07 K.
Paper: Electron Density Distribution in H II Regions in IC 10
Authors: Fiorella L. Polles, Dario Fadda, William D. Vacca, Nicholas P. Abel, Mélanie Chevance, Christian Fischer, James M. Jackson, Vianney Lebouteiller, Suzanne Madden, Lise Ramambason
Figure caption: Theoretical ratio [S III] λ33 μm/[S III] λ18 μm at the temperature of 9700 K as a function of the electron density n e. The symbols indicate the observed line-ratio values. The gray area shows the uncertainty due to the temperature’s uncertainty: the range is between 103.89 and 104.07 K.
Paper: Electron Density Distribution in H II Regions in IC 10
Authors: Fiorella L. Polles, Dario Fadda, William D. Vacca, Nicholas P. Abel, Mélanie Chevance, Christian Fischer, James M. Jackson, Vianney Lebouteiller, Suzanne Madden, Lise Ramambason
Figure caption: SFR vs. n e [O III] (top) and SFR vs. n e [S III] (bottom) for different integrating areas (from left to right, c1, c2, and c3). The color code and symbols are the same as Figure 3. Spearman's rank correlation coefficient is indicated in the top right corner (ρ).
Paper: Electron Density Distribution in H II Regions in IC 10
Authors: Fiorella L. Polles, Dario Fadda, William D. Vacca, Nicholas P. Abel, Mélanie Chevance, Christian Fischer, James M. Jackson, Vianney Lebouteiller, Suzanne Madden, Lise Ramambason
Figure caption: Left: increasing distribution of the 70 μm fluxes, with a zoom on the distribution showing the point where the emission starts to increase rapidly. The black line shows the upper limit of the fluxes used to calculate the foreground emission, while the red line corresponds to the derived foreground emission. Right: map of the continuum 70 μm emission showing only the pixels with a flux higher than the upper limit used to identify the “tail” (black line on the plot on the left).
Paper: Electron Density Distribution in H II Regions in IC 10
Authors: Fiorella L. Polles, Dario Fadda, William D. Vacca, Nicholas P. Abel, Mélanie Chevance, Christian Fischer, James M. Jackson, Vianney Lebouteiller, Suzanne Madden, Lise Ramambason
Figure caption: Left: increasing distribution of the 24 μm fluxes, with a zoom on the distribution showing the point where the emission starts to increase rapidly. The black line shows the upper limit of the fluxes used to calculate the foreground emission, while the red line corresponds to the derived foreground emission. Right: map of the continuum 24 μm emission showing only the pixels with a flux higher than the upper limit used to identify the “tail” (black line on the plot on the left).