Authors: Seiji Fujimoto, Rohan P. Naidu, John Chisholm, Hakim Atek, Ryan Endsley, Vasily Kokorev, Lukas J. Furtak, Richard Pan, Boyuan Liu, Volker Bromm, Alessandra Venditti, Eli Visbal, Richard Sarmento, Andrea Weibel, Pascal A. Oesch, Gabriel Brammer, Daniel Schaerer, Angela Adamo, Danielle A. Berg, Rachel Bezanson, Rychard Bouwens, Iryna Chemerynska, Adélaïde Claeyssens, Miroslava Dessauges-Zavadsky, Anna Frebel, Damien Korber, Ivo Labbe, Rui Marques-Chaves, Jorryt Matthee, Kristen B. W. McQuinn, Julian B. Muñoz, Priyamvada Natarajan, Alberto Saldana-Lopez, Katherine A. Suess, Marta Volonteri, and Adi Zitrin
First Author’s Institution: Department of Astronomy & Astrophysics, University of Toronto
Status: Published in The Astrophysical Journal [open access]
You, me, your laptop, my $8 matcha, and just about everything else on Earth was forged in the fiery bellies of dying stars. Generations of stars had to live and die before the Universe became enriched with any elements heavier than helium (what astronomers call “metals”). The first stars to undergo this cosmic cycle are known as Population III (Pop III) stars. Though their existence has been hypothesized since the 1960s, astronomers have failed to observe these metal-free, distant stars or the faint, low-mass galaxies that host them. The first Pop III stars likely formed around 100 million years after the Big Bang in pristine pockets of hydrogen gas. Although these are too distant for us to observe, we expect that as the Universe started to become metal-enriched, there were still existing pockets of gas introverted enough to survive unpolluted and form metal-free Pop III stars up to a redshift of z~6-7 (when the Universe was around 900 million years old)! The James Webb Space Telescope (JWST) is the perfect instrument to search for these systems. You can read other astrobites on the search for possible Pop III systems with JWST here and here. The authors of today’s paper seek to develop the most efficient way of using JWST’s NIRCam (the near-infrared imager) to find the galaxies hosting Pop III stars. Using their selection method on existing NIRCam data, the authors identified one promising Pop III galaxy candidate.
I’m not like other galaxies
In order to find a Pop III galaxy, we need to take a look at their spectral energy distributions (SEDs). These are graphs that show the energy emitted by a galaxy at different wavelengths of light. Pop III galaxies are expected to have SEDs that differ from your everyday, metal-enriched galaxy. NIRCam will be especially sensitive to three key spectral features that show up in the SEDs of Pop III galaxies: an absent [O III] line (light emitted by doubly ionized oxygen atoms), a strong H-alpha line (light emitted when a hydrogen atom transitions from its third to its second energy level), and a significant Balmer jump (light absorbed to ionize electrons in the second energy level of a hydrogen atom). To identify these key SED characteristics, the authors use SED fitting and color-color diagrams to execute an efficient Pop III search with NIRCam.
The first selection method involves SED fitting. Astronomers create template SEDs that represent different types of galaxies and then compare these templates to the observed SEDs to see which one matches best. In this work, the authors use metal-rich galaxy templates and Pop III templates to fit the galaxies observed with NIRCam. They then calculate the chi-squared χ² (a statistical measure of best fit) between the data and all the SED templates. A galaxy is selected as a Pop III candidate if the Pop III model provides a good fit to the photometry (χ² < 10) and is significantly better than any metal-rich model. It’s kind of like looking for Cinderella by making every woman in the kingdom try on the glass slipper.
A color-color diagram plots the difference in magnitude between two filters on each axis. NIRCam filters are specially chosen to emphasize the SED characteristics above. When these filters are chosen, Pop III galaxies occupy a distinct region of this diagram as compared to metal-rich galaxies. For example, subtracting the F356W filter from the F277W filter is sensitive to the presence of the OIII line and the Balmer jump. Figure 1 demonstrates how this color selection separates Pop III from typical galaxies.
O Pop III, Pop III wherefore art thou?
The authors apply their fresh, new selection criteria to publicly available NIRCam data from large surveys. And (drum roll please) the slipper fits! The Pop III galaxy candidate GLIMPSE-16043 is an ultra-faint galaxy at z=6.5. It was imaged in the GLIMPSE survey, which uses the technique of gravitational lensing to better observe faint and distant galaxies. The GLIMPSE survey targeted a massive galaxy cluster, Abell S1063. The cluster bends the light from distant galaxies and, like a giant lens, magnifies far-away objects, providing some of the deepest JWST imaging to date. The Pop III candidate passes both tests: it resides in the Pop III region of the color-color diagram, and its SED is best fit by a Pop III model, not a metal-rich galaxy model (see Figure 2). Next, spectroscopic follow-up is needed to ensure that this galaxy is truly metal-free and not just extremely metal-poor.
The authors conclude that our best shot at identifying additional Pop III galaxy candidates is using NIRCam to image large numbers of gravitationally lensed clusters. Without magnification from gravitational lensing, it may be impossible to see these ultra-faint Pop III galaxies. Once candidates have been identified, they can be followed up with deep spectroscopy to confirm their redshift and their lack of metals. Who knows? With these new methods, we may soon get a glimpse of the Universe’s very first stars.
Astrobite edited by Chris Layden and Margaret Verrico
Featured image credit: NOIRLab/NSF
