The X-ray Integral Field Unit (X-IFU) is the cryogenic micro-calorimeter of the Athena space X-ray observatory, the second large mission of the Cosmic Vision Program of the European Space Agency, selected to explore the scientific theme “The Hot and Energetic Universe”. It is designed to 1) study the dynamical, physical and chemical properties of hot plasmas, as those found in clusters of galaxies, and 2) study black hole accretion disks, jets, outflows and winds from galactic stellar mass black holes to the super-massive ones found in active galactic nuclei. With its unprecedented capabilities, it is also the prime instrument for many Athena observatory science targets, such as planets, stars, supernovae, compact objects, interstellar medium among many other scientific topics.
X-IFU is a cryogenic imaging spectrometer, offering spatially-resolved high-spectral resolution X-ray spectroscopy over a 5 arc minute equivalent diameter field of view with spectral resolution of 2.5 eV up to 7 keV. The breadth of the science affordable with the X-IFU encompasses key scientific issues of the Hot and Energetic Universe science theme and beyond.
NASA’s James Webb Space Telescope is unloaded from a U.S. military C-5 Charlie aircraft at Los Angeles International Airport (LAX) on Feb. 2, 2018. Credits: NASA/Chris Gunn
The optics and scientific instrumentation (OTIS) of JWST arrived yesterday in the facilities
of Northrop Grumman in California, where the rest of the spacecraft (solar shields, communication elements, etc) is already. The OTIS passed the final performance tests
last year at NASAS’s Johnson Space Center in Houston, Texas. The spacecraft bus
and solar shields still need to perform a series of tests before the integration, however. Continue reading →
The MIRI Medium-Resolution Spectrometer (MRS) is the only mid-IR Integral Filed Spectrograph on board the James Webb Space Telescope. It offers integral field spectroscopy at resolutions up to ~4000, between 4.9 and 28.8 μm using four different nested Integral Field Units up to 7.2″ × 7.9″ in size. This workshop is part of a series of conferences of meetings of the international MRS testing and calibration working group. With these periodic workshops we define commissioning activities and calibration products to deliver to guarantee the best scientific return of MRS. Continue reading →
HST image and GTC/OSIRIS spectra of the “Teacup” containing the Hα+[NII] lines. We highlight prominent emission line features such as the NE and SW bubbles. For further details, see Villar-Martín et al. 2017.
The “Teacup” (SDSS J143029.88+133912.0 at z=0.085) is a nearby quasar, whose nickname comes from the peculiar morphology of the extended ionized gas. It shows a loop-shaped structure reminiscent of a teacup “`handle” which extends up to ~12 kpc (~39,000 light years) NE of the active galactic nucleus. Continue reading →
Left: Map of the 448 GHz (rest frequency) continuum (top panel) and zeroth moment of the H2O 423 − 330 emission (bottom panel) of ESO 320-G030. Right: Continuum subtracted profile of the H2O 423 − 330 448 GHz emission. See Pereira-Santaella et al. 2017 for further details.
Water is a key molecule to probe dense and warm regions in the interstellar medium, because of its chemistry as well as its coupling to the far-infrared. This work presents the first detection of the ortho-H2O 4_23 – 3_30 transition at 448 GHz in space. Continue reading →
Artist impression illustrating a super-massive black hole with X-ray emission emanating from its inner region (pink) and ultrafast winds streaming from the surrounding disk (purple). Credit: ESA
Active Galactic Nuclei (AGN) are thought to have a profound effect on large scales through feedback mechanisms. AGN gas outflows release vast amounts of energy into the interstellar medium and can clear out the surrounding gas, possibly regulating star formation in the host galaxy as well as preventing further gas accretion onto the black hole. Such feedback may well contribute to the intimate observed relationship between the central black hole and the host galaxy properties.
Molecular gas on multiple scales in the Spiderweb galaxy
The largest galaxies in the universe reside in galaxy clusters. Using sensitive observations of carbon monoxide, we show that the Spiderweb galaxy—a massive galaxy in a distant protocluster—is forming from a large reservoir of molecular gas. Most of this molecular gas lies between the protocluster galaxies and has low velocity dispersion, indicating that it is part of an enriched intergalactic medium. This may constitute the reservoir of gas that fuels the widespread star formation seen in earlier ultraviolet observations of the Spiderweb galaxy. Our results support the notion that giant galaxies in clusters formed from extended regions of recycled gas at high redshift.
In support of activities related to the NIRSpec instrument on the James Webb Space Telescope (JWST), a contract at the postdoctoral research level is offered at the Astrophysics Department of the Center for Astrobiology (CAB), in Madrid. Continue reading →
The dust continuum emission at 694 GHz mapped by ALMA in the circumnuclear disk of NGC1068. See García-Burillo et al. 2016 for further details.
An international team of astronomers lead by the spanish astronomer Santiago García-Burillo (OAN, Madrid), and with the participation of CAB scientists (Almudena Alonso Herrero and Luis Colina), have been able to resolve for the first time the dusty torus around the massive black hole in the nucleus of the nearby active galaxy NGC 1068.