Pursuing the Firstborn Stars and a Better Cosmic Creation Model

Pursuing the Firstborn Stars and a Better Cosmic Creation Model

Elusive detection of the universe’s firstborn stars has been a long-standing challenge toward developing a more detailed and better affirmed biblically predicted big bang creation model.1 Astronomers call them Population III stars, and a failure to observe them has led some people to conclude that the big bang creation model has been falsified. For example, past president of the Institute for Creation Research, Henry Morris II, wrote,

The problem is that, out of the billions upon billions of stars in the observable universe, there do not seem to be any Type-3 Stars [Population III stars] at all. . . . It seems like we should see plenty of them if they ever existed, since all the other stars supposedly keep coming from them.2

John Hartnett, Rod Bernitt, and Jonathan Sarfati of Creation Ministries International respectively wrote,

These original stars have never been observed, hence they were nothing more than hypothetical. . . . It [the Big Bang model] vitally needs those Population III stars or there is no story.3 Their existence [of Population III stars] remains a matter of conjecture, not fact.4 The total absence of these stars counts as a falsified prediction of Big Bang cosmology.5

They base their critiques on the notion that in big bang cosmology the universe begins with only two elements, hydrogen and helium, and just a trace amount of lithium (with atomic weights of 1, 4, and 7, respectively). Therefore, the firstborn stars will possess no elements heavier than lithium. So far, the spectra of all observed stars reveal elements heavier than helium. (In a star’s spectrum astronomers see a star’s different colors of light and learn what a star is made of.)

Detection Difficulties
The irony in these critics’ assertions is that they overlooked the fact that the big bang creation model predicts that the spectra of the universe’s firstborn stars would be undetectable by present-day telescope power. Most big bang creation models predict that all Population III stars will be supergiant stars, stars larger than 20 times the mass of the Sun. Such stars will burn up in just several million years or less. Thus, they will be bright only in the very early history of the universe. Astronomers will see them only if they search for them at distances greater than 13.5 billion light-years away. No existing telescope has the power to measure the spectrum of a star at such a great distance.

A few big bang creation models predict that while most Population III stars will be supergiants, a small percentage may be stars 1–20 times the Sun’s mass, and a very tiny percentage may be as small as 0.8 times the Sun’s mass. Stars less than 0.8 times the Sun’s mass will burn for more than 13.5 billion years. Therefore, one or more of them might burn long enough to be close enough that astronomers can measure their spectra.

Such old Population III stars, however, will not be pristine. Their initial elemental makeup of only hydrogen, helium, and a trace amount of lithium will be contaminated by their atmospheres accreting small quantities of elements heavier than helium from the ashes of exploded supergiant Population III stars and ashes from the later-formed supergiant Population II stars. This contamination, though, will be minimized for old, low-mass Population III stars that have permanently resided in regions where the stellar density is very low.

New Spectral Measurements
Where spectral measurements reveal that this contamination is exceptionally low, specific details in the spectrum can reveal the precise source of the contamination and, therefore, positively determine whether or not the contaminated star is a true Population III star. A team of nine astronomers led by Rana Ezzeddine and Anna Frebel recently performed such measurements on the old star HE 1327-2326 to provide strong evidence that HE 1327-2326 is indeed a true Population III star that was contaminated more than 13 billion years ago by the nearby aspherical supernova explosion of a single high-mass Population III star.6

A team of nineteen astronomers led by Anna Frebel discovered HE 1327-2326 in 2005.7 They found it in the outer halo of our Milky Way Galaxy, a region where the density of stars is very low. HE 1327-2326’s mass is 0.8 times the Sun’s mass and its spectral features reveal it has completed its main sequence history of stellar burning.8 Therefore, HE 1327-2326 likely is older than 13 billion years. In the discovery paper, Frebel’s team found that HE 1327-2326 had the lowest abundance of elements heavier than helium of any known star. Its ratio of iron to hydrogen measured to be only 1/250,000th of the Sun’s.9

Today, HE 1327-2326 ranks as the star with the second lowest known abundance of elements heavier than helium. The recently discovered star SDSS J102915+172927 has an iron to hydrogen ratio less than 1/10,000,000th the Sun’s.10

Unlike SDSS J102915+172927, HE 1327-2326 is not deficient in carbon. This feature led Ezzeddine and Frebel’s team to consider that HE 1327-2326 may be a low-mass Population III star that was externally enriched by the debris from a single high-mass Population III star that underwent an aspherical supernova explosion (see figure 1). To test their hypothesis, Ezzeddine and Frebel’s team used the Hubble Space Telescope to observe the ultraviolet spectrum (2,118–2,348 angstroms) of HE 1327-2326 for a total integration time of 22 hours and 20 minutes. For the first time ever, they got accurate measurements in this wavelength range of seven spectral lines of HE 1327-2326: one zinc line, five iron lines, and one silicon line.

Figure 1: Artist’s Rendition of an Aspherical Supernova Explosion. Image credit: NASA/CXC/M. Weiss

Observing Population III Stars
Armed with the new spectral measurements, Ezzeddine, Frebel, and their colleagues showed that the entire abundance pattern of HE 1327-2326 is explained by its being a Population III star that was blasted by one of the jets from a “rotation driven, high-energy (E = 5 x 1051 erg) aspherical SNe [supernova eruption] with bipolar jets”11 of a 25-solar-mass Population III star. Therefore, Ezzeddine and Frebel’s team established the existence of not just one, but two Population III stars.

Meanwhile, a team of Japanese astronomers has published two papers in which they demonstrate that astronomers may not need to wait for future super telescopes—like the James Webb Space Telescope or ground-based telescopes with mirror diameters larger than 30 meters (100 feet)—to directly detect high-mass Population III stars. The team shows that the near-infrared imaging capability of the 8.2-meter-diameter Subaru Telescope (see figure 2) combined with the natural magnification afforded by the gravitational lensing of intervening massive galaxy clusters may detect extremely distant massive Population III stars undergoing pair-instability supernova eruptions.12

Figure 2: Subaru Telescope on Top of Mauna Kea in Hawaii. Image credit: Denys, Creative Commons Attribution

Already, the fact that Ezzeddine and Frebel’s team has established the existence of both high- and low-mass Population III stars will help astronomers develop a more detailed and specified big bang creation model. Such an advance will provide even stronger evidence for what the Bible had uniquely predicted about the universe thousands of years ago.

  1. Hugh Ross and John Rea, “Big Bang—The Bible Taught It First!” RTB 101 (June 30, 2000), https://www.reasons.org/explore/publications/rtb-101/read/rtb-101/2000/06/30/big-bang-the-bible-taught-it-first.
  2. Henry M. Morris II, “The Stardust Trail,” Acts & Facts 28, no. 1 (January 1999), https://www.icr.org/article/stardust-trail.
  3. John G. Hartnett, “Have Population III Stars Finally Been Discovered?” Creation Ministries International, (blog), March 3, 2016, https://creation.com/have-population-iii-stars-been-discovered.
  4. Rod Bernitt, “Stellar Evolution and the Problem of the ‘First’ Stars,” Journal of Creation 16, no. 1 (April 2002): 12–14, https://creation.com/stellar-evolution-and-the-problem-of-the-first-stars.
  5. Jonathan Sarfati, Refuting Compromise: A Biblical and Scientific Refutation of Progressive Creationism, As Popularized by Astronomer Hugh Ross, 2nd ed. (Atlanta: Creation Book Publishers, 2011), 161.
  6. Rana Ezzeddine et al., “Evidence for an Aspherical Population III Supernova Explosion Inferred from the Hyper-Metal-Poor Star HE 1327-2326,” Astrophysical Journal 876, no. 2 (May 10. 2019): id. 97, doi:10.3847/1538-4357/ab14e7.
  7. Anna Frebel et al., “Nucleosynthetic Signatures of the First Stars,” Nature 434 (April 14, 2005): 871–873, doi:10.1038/nature03455.
  8. Frebel et al., “Nucleosynthetic Signatures,” 871.
  9. Frebel et al., “Nucleosynthetic Signatures,” 871.
  10. S. C. Keller et al., “A Single Low-Energy, Iron-Poor Supernova As the Source of Metals in the Star SMSS J03100.36-670839.3,” Nature 506 (February 9, 2014): 463–66, doi:10.1038/nature12990.
  11. Ezzeddine et al., “Evidence for an Aspherical,” 7.
  12. Takashi J. Moriya et al., “Searches for Population III Pair-Instability Supernovae: Predictions for ULTIMATE-Subaru and WFIRST,” Publications of the Astronomical Society of Japan 71, no. 3 (June 2019): id. 59, doi:10.1093/pasj/psz035; Kenneth C. Wong et al., “Searches for Population III Pair-Instability Supernovae: Impact of Gravitational Lensing Magnification,” Publications of the Astronomical Society of Japan 71, no. 3 (June 2019): id. 60, doi:10.1093/pasj/psz037.