This color-composite shows a main part of the new Blanco DECam Bulge Survey of 250 million stars in our galaxy’s bulge. The 4 x 2 degrees excerpt can be explored in all its whopping 50,000 x 25,000 pixels in the zoomable version. In the image interstellar dust and gas seemingly acts like a red “filter” in front of the background stars, scattering the blue light away. Since we are surrounded by dust and gas in the Milky Way, this scattering effect is important to many parts of astronomy and is known as interstellar reddening. Credit: CTIO/NOIRLab/DOE/NSF/AURA, Acknowledgment: Image processing: W. Clarkson (UM-Dearborn), C. Johnson (STScI), and M. Rich (UCLA), Travis Rector (University of Alaska Anchorage), Mahdi Zamani & Davide de Martin.
Star-studded image shows the glittering central parts of the Milky Way
For the first time, over 250 million stars in our galaxy’s bulge have been surveyed in near-ultraviolet, optical, and near-infrared light, opening the door for astronomers to reexamine key questions about the Milky Way’s formation and history. Using ultraviolet data, and with 450,000 individual images, the team was able to measure the chemical composition of tens of thousands of stars spanning a large area of the bulge. The vast dataset can be explored in spectacular detail in this image.
The mysteries of the Milky Way are revealed in spectacular detail, thanks to the efforts of a team of astronomers who have observed 250 million stars in the bulge at the heart of the Milky Way using the Dark Energy Camera (DECam). DECam, primarily funded by the U.S. Department of Energy, is mounted on the Víctor M.Blanco 4-meter Telescope at the Cerro Tololo Inter-American Observatory (CTIO) in Chile, a program of NSF’s NOIRLab. By detecting the ultraviolet light from stars in the bulge known as Red Clump stars, they were able to analyze the chemical composition of over 70,000 stars over an area of sky 1,000 times as large as the full Moon (an area larger than 20 x 10 degrees stretching over the constellations Sagittarius and Scorpius).
This image of a region near the center of the Milky Way galaxy covers 0.5 by 0.25 degrees on the sky (an area about twice as wide as the full Moon) and contains over 180,000 stars. The image captures a portion of our galaxy about 220 by 110 light-years across. It was taken with the Dark Energy Camera on the Víctor M. Blanco 4-meter Telescope at the Cerro Tololo Inter-American Observatory in Chile, a Program of NSF’s NOIRLab. By studying the brightnesses of these stars at different wavelengths of light, astronomers were able to determine how many heavy elements they contain, which is related to their formation history. Credit: CTIO/NOIRLab/DOE/NSF/AURA/STScI, W. Clarkson (UM-Dearborn), C. Johnson (STScI), and M. Rich (UCLA)
The data are hosted and served to the community by NOIRLab’s Community Science and Data Center (CSDC), also a program of NSF’s NOIRLab, which handled the more than 7,000 DECam exposures, comprising more than 3.5 trillion pixels. A color-composite showing a main part of these data is shown in this image, and can be explored in all its whopping 50,000 x 25,000 pixels in this zoomable version.
The newly published study has shown that the stars near the very center of the Milky Way have a very similar composition, which suggests that they formed at around the same time. Normally composition is measured with a spectrograph, targeting a relatively small number of stars at a time (although the revolutionary DESI instrument at Kitt Peak National Observatory, a program of NSF’s NOIRLab, will soon be able to do thousands). However, the Blanco DECam Bulge Survey took a different approach and instead precisely measured the stars’ brightness differences from ultraviolet to infrared wavelengths. These differences in brightness at different wavelengths are called photometric colors by astronomers, and can reveal the composition of stars when the dataset is calibrated with stars measured spectroscopically.
This image shows a wide-field view of the center of the Milky Way with a pull-out image of the Dark Energy Camera (DECam) at the Cerro Tololo Inter-American Observatory in Chile, a Program of NSF’s NOIRLab. The DECam image covers around 4 x 2 degrees (an area about 8 times as wide as the full Moon). Credit: CTIO/NOIRLab/DOE/NSF/AURA/STScI, W. Clarkson (UM-Dearborn), C. Johnson (STScI), and M. Rich (UCLA)/E.Slawik
The team used DECam’s three square degree field of view to take over 450,000 individual images, before focusing on the subsample of 70,000 stars, which is substantially larger than previous spectroscopic bulge surveys. Future work with the full DECam data set will yield millions of composition measurements, a sample size more than 200 times that of even the largest spectroscopic surveys.
Kathy Vivas, co-author and NOIRLab astronomer said, “This is exactly the strength of the Dark Energy Camera — to undertake these kinds of studies. While it was originally aimed at the study of the distant Universe to measure its expansion, DECam has proven to be a powerful instrument to study our Milky Way as well.”
The survey results are providing key insights into the formation of the bulge and a glimpse of what is to come when the upcoming Vera C. Rubin Observatory begins acquiring its own images of the Milky Way. “Many other spiral galaxies look like the Milky Way and have similar bulges, so if we can understand how the Milky Way formed its bulge then we’ll have a good idea of how the other galaxies did too,” said study co-leader Christian Johnson of Space Telescope Science Institute.
These data would also surely have fascinated Víctor M. Blanco and his wife Betty Blanco, after whom the Blanco DECam Bulge Survey is named. Almost 50 years ago they used the same telescope to explore, amongst other things, the Milky Way’s bulge. Half a century later, our home galaxy has plenty of surprises to offer.
The Víctor M. Blanco 4-meter Telescope has a 4-meter (13 feet) diameter mirror, which weighs 15,400 kg (34,000 lbs). It was designed in the 1960’s. The Dark Energy Camera (black paint) is mounted at the prime (first) focus near the top of the Serrurier truss (white paint). The blue-painted structure is the large bearing that allows the telescope to move in right ascension. The telescope declination axis is located at the level of the middle of the right ascension bearing and is best seen on the left side of the large u-shaped notch. The primary mirror is located a few feet lower than the declination axis. Credit: DOE/LBNL/DECam/R. Hahn/CTIO/NOIRLab/NSF/AURA
This research was presented in two papers that appeared in the journal Monthly Notices of the Royal Astronomical Society.
“The Blanco DECam bulge survey. I. The survey description and early results” by R Michael Rich, Christian I Johnson, Michael Young, Iulia T Simion, William I Clarkson, Catherine Pilachowski, Scott Michael, Andrea Kunder, A Katherina Vivas, Andreas Koch, Tommaso Marchetti, Rodrigo Ibata, Nicolas Martin, Annie C Robin, Nadége Lagarde, Michelle Collins, Željko Ivezić, Roberto de Propris, Juntai Shen, Ortwin Gerhard and Mario Soto, 18 August 2020, Monthly Notices of the Royal Astronomical Society.
“Blanco DECam Bulge Survey (BDBS) II: project performance, data analysis, and early science results” by Christian I Johnson, Robert Michael Rich, Michael D Young, Iulia T Simion, William I Clarkson, Catherine A Pilachowski, Scott Michael, Andrea Kunder, Andreas Koch and Anna Katherina Vivas, 3 September 2020, Monthly Notices of the Royal Astronomical Society.
The team involved is composed of R. Michael Rich (University of California, Los Angeles), Christian I. Johnson (Space Telescope Science Institute), Michael Young (Indiana University), Iulia T. Simion (Shanghai Astronomical Observatory), William I. Clarkson (University of Michigan-Dearborn), Catherine Pilachowski (Indiana University), Scott Michael (Indiana University), Andrea Kunder (St Martin’s University), A. Katherina Vivas (NSF’s NOIRLab), Andreas Koch (University of Heidelberg), Tommaso Marchetti (European Southern Observatory), Rodrigo Ibata (Strasbourg Observatory), Nicolas Martin (Strasbourg Observatory), Annie C. Robin (University of Bourgogne Franche-Comté), Nadége Lagarde (University of Bourgogne Franche-Comté), Michelle Collins (University of Surrey), Željko Ivezic (University of Washington), Roberto de Propris (Finnish Centre for Astronomy with ESO), and Juntai Shen (Shanghai Jiao Tong University).
NSF’s NOIRLab (National Optical-Infrared Astronomy Research Laboratory), the US center for ground-based optical-infrared astronomy, operates the international Gemini Observatory (a facility of NSF, NRC–Canada, ANID–Chile, MCTIC–Brazil, MINCyT–Argentina, and KASI–Republic of Korea), Kitt Peak National Observatory (KPNO), Cerro Tololo Inter-American Observatory (CTIO), the Community Science and Data Center (CSDC), and Vera C. Rubin Observatory (in cooperation with DOE’s SLAC National Accelerator Laboratory). It is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with NSF and is headquartered in Tucson, Arizona. The astronomical community is honored to have the opportunity to conduct astronomical research on Iolkam Du’ag (Kitt Peak) in Arizona, on Maunakea in Hawaiʻi, and on Cerro Tololo and Cerro Pachón in Chile. We recognize and acknowledge the very significant cultural role and reverence that these sites have to the Tohono O’odham Nation, to the Native Hawaiian community, and to the local communities in Chile, respectively.