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Webb y el Hubble se unen para rastrear el polvo interestelar: “Tenemos más de lo que esperábamos”

Al combinar datos del Telescopio Espacial James Webb de la NASA y el Telescopio Espacial Hubble de la NASA, los investigadores pudieron rastrear la luz emitida por la gran galaxia elíptica blanca de la izquierda a través de la galaxia espiral de la derecha. Como resultado, pudieron identificar los efectos del polvo interestelar en la galaxia espiral. Los datos del infrarrojo cercano de Webb también nos muestran los brazos espirales más largos y extremadamente polvorientos de la galaxia con mucho más detalle, lo que les da la apariencia de superponerse con el bulto central de la brillante galaxia elíptica blanca de la izquierda, aunque el par no está interactuando. En esta imagen, el verde, el amarillo y el rojo se asignaron a los datos del infrarrojo cercano de Webb tomados en 0,9, 1,5 y 3,56 micrones (F090W, F150W y F356W, respectivamente). El azul se asignó a dos filtros Hubble, los datos ultravioleta se tomaron en 0,34 micras (F336W) y la luz visible en 0,61 micras (F606W).
Crédito: Ciencia: NASA, ESA, CSA, Rogier Windhorst (ASU), William Keel (Universidad de Alabama), Stuart Wyithe (Universidad de Melbourne), Equipo JWST PEARLS, Procesamiento de imágenes: Alyssa Pagan (STScI)

“Obtuvimos más de lo que esperábamos al combinar datos de

Establecida en 1958, la Administración Nacional de Aeronáutica y del Espacio (NASA) es una agencia independiente del Gobierno Federal de los Estados Unidos que sucedió al Comité Asesor Nacional para la Aeronáutica (NACA). Es responsable del programa espacial civil, así como de la investigación aeronáutica y aeroespacial. Su visión es “Descubrir y expandir el conocimiento en beneficio de la humanidad.” Sus valores fundamentales son “seguridad, integridad, trabajo en equipo, excelencia e inclusión.”

” data-gt-translate-attributes=”[{” attribute=””>NASA’s elliptical galaxy, at left, through the winding spiral galaxy at right – and identify the effects of interstellar dust in the spiral galaxy. This image of galaxy pair, known as VV 191, includes near-infrared light from Webb, and ultraviolet and visible light from Hubble.

With Webb’s near-infrared data we can see the galaxy’s longer, extremely dusty spiral arms in far more detail. It gives the arms an appearance of overlapping with the central bulge of the bright white elliptical galaxy on the left. While the two foreground galaxies are relatively close astronomically speaking, they are not actively interacting.

VV 191 is the latest addition to a small number of galaxies that helps researchers directly compare the properties of galactic dust. This target was selected from nearly 2,000 superimposed galaxy pairs identified by Galaxy Zoo citizen science volunteers.

Because dust changes the brightness and colors that appear in images of the galaxies, it is important to understand where dust is present in them. Since dust grains are partially responsible for the formation of new stars and planets, astronomers are always striving to identify their presence for further investigations.

Lensed Galaxies in VV 191

Researchers identified a previously unknown lensed galaxy for the first time in new near-infrared data from NASA’s James Webb Space Telescope. Above the white elliptical galaxy at left, a faint red arc appears in the inset at 10 o’clock. This is a very distant galaxy whose appearance is warped. Its light is bent by the gravity of the elliptical foreground galaxy. Plus, its appearance is duplicated. The stretched red arc is warped where it reappears – as a dot – at 4 o’clock. In this image, green, yellow, and red were assigned to Webb’s near-infrared data taken in 0.9, 1.5, and 3.56 microns (F090W, F150W, and F356W respectively). Blue was assigned to two Hubble filters, ultraviolet data taken in 0.34 microns (F336W) and visible light in 0.61 microns (F606W).
Credit: Science: NASA, ESA, CSA, Rogier Windhorst (ASU), William Keel (University of Alabama), Stuart Wyithe JWST PEARLS Team, Image Processing: Alyssa Pagan (STScI)

The image also holds a second discovery that’s easier to overlook. Carefully examine the white elliptical galaxy at left. A faint red arc appears in the inset at 10 o’clock. This arc is a very distant galaxy whose light is bent by the gravity of the elliptical foreground galaxy – and its appearance is duplicated. The stretched red arc is warped where it reappears – as a dot – at 4 o’clock. Because these images of the lensed galaxy are so faint and so red that they went unrecognized in Hubble data. However, they are unmistakable in Webb’s near-infrared image. Simulations of gravitationally lensed galaxies like this help astronomers reconstruct how much mass is in individual stars, as well as how much dark matter is in the core of this galaxy.

As with many images from the James Webb Space Telescope, this image of VV 191 shows additional galaxies deeper and deeper in the background. Two patchy spirals to the upper left of the elliptical galaxy have similar apparent sizes, but show up in very different colors. One is likely very dusty and the other very far away, but astronomers will need to obtain data known as spectra to determine which is which.


“Webb’s PEARLS: dust attenuation and gravitational lensing in the backlit-galaxy system VV 191” by William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Norman A. Grogin, Christopher N.A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan Jr., Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S.P. Willner, Andreea Petric, Cheng Cheng and Adi Zitrin, 30 August 2022, Astrophysics > Astrophysics of Galaxies.

“Webb’s PEARLS: Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results” by Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Scott Tompkins, Christopher J. Conselice, Simon P. Driver, Haojing Yan, Dan Coe, Brenda Frye, Norman Grogin, Anton Koekemoer, Madeline A. Marshall, Nor Pirzkal, Aaron Robotham, Russell E. Ryan Jr., Christopher N. A. Willmer, Timothy Carleton, Jose M. Diego, William C. Keel, Rosalia O’Brien, Paolo Porto, Caleb Redshaw, Sydney Scheller, Andi Swirbul, Stephen M. Wilkins, S. P. Willner, Adi Zitrin, Nathan J. Adams, Duncan Austin, Richard G. Arendt, John F. Beacom, Rachana A. Bhatawdekar, Larry D. Bradley, Thomas J. Broadhurst, Cheng Cheng, Francesca Civano, Liang Dai, Herve Dole, Jordan C. J. D’Silva, Kenneth J. Duncan, Giovanni G. Fazio, Giovanni Ferrami, Leonardo Ferreira, Steven L. Finkelstein, Lukas J. Furtak, Alex Griffiths, Heidi B. Hammel, Kevin C. Harrington, Nimish P. Hathi, Benne W. Holwerda, Jia-Sheng Huang, Minhee Hyun, Myungshin Im, Bhavin A. Joshi, Patrick S. Kamieneski, Patrick Kelly, Rebecca L. Larson, Juno Li, Jeremy Lim, Zhiyuan Ma, Peter Maksym, Giorgio Manzoni, Ashish Kumar Meena, Stefanie N. Milam, Mario Nonino, Massimo Pascale, Justin D. R. Pierel, Andreea Petric, Maria del Carmen Polletta, Huub J. A. Rottgering, Michael J. Rutkowski, Ian Smail, Amber N. Straughn, Louis-Gregory Strolger, James A. A. Trussler, Lifan Wang, Brian Welch, J. Stuart B. Wyithe, Min Yun, Erik Zackrisson, Jiashuo Zhang and Xiurui Zhao, 9 September 2022, Astrophysics > Cosmology and Nongalactic Astrophysics.

Webb interdisciplinary scientist Rogier Windhorst of Arizona State University and his team obtained the data used in this image from early results of the Prime Extragalactic Areas for Reionization and Lensing Science (PEARLS) JWST Guaranteed Time Observation (GTO) programs, GTO 1176 and 2738. Additional data from Hubble’s STARSMOG snapshot program (SNAP 13695) and GO 15106, were added. Jake Summers, also of Arizona State, performed the pipeline data reduction. The dust analysis was led by William Keel of the University of Alabama, while the Hubble data acquisition was led by Benne Holwerda of the University of Louisville in Kentucky. The detailed gravitational-lensing analysis was conducted by Giovanni Ferrami and Stuart Wyithe, both of the University of Melbourne, Australia and ASTRO 3D, Australia.

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