Search

Image Details

View Article Bookmark & Share

Choose export citation format:

Export Citation
Large resolution
Hi-Resolution Export to PDF

A SPHEREx Pipeline and Spectral Library for Ultracool Dwarfs

  • Authors: Jonathan Gagné, Jacqueline K. Faherty, Azul Ruiz Diaz, Louis-Philippe Coulombe, Thomas P. Bickle, Adam C. Schneider, J. Davy Kirkpatrick, Marc J. Kuchner, Aaron M. Meisner, Dan Caselden, Adam J. Burgasser, Sarah Casewell, Easton J. Honaker, Frank Kiwy, Federico Marocco, Daniella C. Bardalez Gagliuffi, Nikolaj Stevnbak Andersen, Lizzeth Ruiz Arroyo, Bruce Baller, Paul Beaulieu, John Bell, Martin Bilsing, Troy K. Bohling, Guillaume Colin, Giovanni Colombo, Sam Deen, Alexandru Dereveanco, Kevin Dixon, Hugo A. Durantini Luca, Deiby Flores, Christoph Franck, Christopher Fulvi, Michael Gallmann, Jean Marc Gantier, Konstantin Glebov, Léopold Gramaize, Leslie K. Hamlet, Ken Hinckley, Kevin Jablonski, Peter A. Jałowiczor, Martin Kabatnik, Peter Kasprowitz, K Ly, David W. Martin, Naoufel Marzak, Alexander McColgan, Neil J. McEwan, Marianne N. Michaels, William Pendrill, Stéphane Perlin, Benjamin Pumphrey, James Rabe, Henry Raway, Walter Ruben Robledo, David Roser, Animesh Roy, Arttu Sainio, Vincent Schindler, Manfred Schonau, Jörg Schümann, Karl Selg-Mann, Andrea Serio, Patrick Smith, Andres Stenner, Christopher Tanner, Melina Thévenot, Vinod Thakur, Mayahuel Torres Guerrero, Maurizio Ventura, Nikita V. Voloshin, Jim Walla, Zbigniew Wȩdracki, Bailey Weyandt, Breck Wilhite, Spartacus Zitouni

Jonathan Gagné et al 2026 The Astrophysical Journal 1009 .

  • Provider: AAS Journals

Caption: Figure 2.

Left panel: histogram of MOCAdb spectral types for known confirmed and candidate ultracool dwarfs. Right panel: WISE W2 magnitudes as a function of spectral types for known confirmed and candidate ultracool dwarfs. Known UCD candidates are concentrated at early L spectral types and magnitudes brighter than W2≈15 because they were mostly uncovered using the individual-epoch detections in the WISE mission (which reaches a 5σ depth of 15.5 in W2 band; E. L. Wright et al. 2010), which samples a much larger volume in space for warmer and intrinsically brighter early-L dwarfs. See Section 3 for more details.

Other Images in This Article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article

Show More

Copyright and Terms & Conditions

Additional terms of reuse