First accurate measurement of the temperature of ancient CMB

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<p><strong>From over-week-old-news-dept:</strong></p><p>The paper: First detection of CO in a high-redshift DLA </p><p>News: http://www.spaceref.com/news/viewpr.html?pid=25428</p><p>&nbsp;</p><p><font face="geneva,arial,verdana" size="+1"><strong> A Molecular Thermometer for the Distant Universe</strong></font></p><p><font face="geneva,arial,verdana" size="-1"><strong>(ESO) First accurate measurement of the temperature of the cosmic background at an early epoch</strong></font> </p><p>&nbsp;</p><p align="left"> <font face="geneva,arial,verdana" size="-1">Astronomers have made use of ESO's Very <font style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" color="blue"><span style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" class="kLink">Large </span><span style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" class="kLink">Telescope</span></font> to detect for the first time in the ultraviolet the carbon monoxide molecule in a galaxy located almost 11 billion light-years away, a feat that had remained elusive for 25 years. This detection allows them to obtain the most precise measurement of the cosmic temperature at such a remote epoch. </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">The team of astronomers [1] aimed the UVES spectrograph on ESO's VLT for more than 8 hours at a well-hidden galaxy whose light has taken almost 11 billion years to reach us, that is about 80% of the age of the Universe. </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">The only way this galaxy can be seen is through the imprint its interstellar gas leaves on the spectrum of an even more remote quasar [2]. "<font style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" color="blue"><span style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" class="kLink">Quasars</span></font> are here only used as a beacon in the very distant Universe. Interstellar clouds of gas in galaxies, located between the quasars and us on the same line of sight, absorb parts of the light emitted by the quasars. The resulting spectrum consequently presents dark 'valleys' that can be attributed to well-known elements and possibly molecules," explains Raghunathan Srianand (Pune, India), who led the team making the observations. </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">Thanks to the power of the VLT and a very careful selection of the target - the target was selected among about ten thousands quasars - the team was able to discover the presence of normal and deuterated molecular <font style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" color="blue"><span style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" class="kLink">hydrogen</span></font> (H2, HD) and carbon monoxide (CO) molecules in the interstellar medium of this remote galaxy. "This is the first time that these three molecules have been detected in absorption in front of a quasar, a detection that has remained elusive for more than a quarter century," says Cedric Ledoux (ESO), member of the team. </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">The same team had already broken the record for the most distant detection of molecular hydrogen in a galaxy that we see as it was when the Universe was less than 1.5 billion years old (see ESO 16/06). </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">The interstellar gas is the reservoir from which stars form and, as such, is an important component of galaxies. Furthermore, because the formation and the state of molecules are very sensitive to the physical conditions of the gas, which in turn depend on the rate at which stars are formed, the detailed study of the chemistry of the <font style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" color="blue"><span style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" class="kLink">interstellar </span><span style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" class="kLink">medium</span></font> is an important tool to understand how galaxies form. </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">Based on their observations, the astronomers showed that the physical conditions prevailing in the interstellar gas in this remote <font style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" color="blue"><span style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" class="kLink">galaxy</span></font> are similar to what is seen in our Galaxy, the Milky Way. </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">But most importantly, the team was able to measure with the best ever precision the temperature of the cosmic background radiation in the remote Universe [3]. "Unlike other methods, measuring the temperature of the cosmic background using the CO molecule involves very few assumptions," declares co-author Pasquier Noterdaeme. </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">If the Universe was formed in a 'Big Bang', as most astrophysicists infer, the glow of this primeval fireball should have been warmer in the past. This is exactly what is found by the new measurements. "Given the current measured temperature of 2.725 K, one would expect that the temperature 11 billion years ago was about 9.3 K," says co- author Patrick Petitjean. "Our unique set of VLT observations allows us to deduce a temperature of 9.15 K, plus or minus 0.7 K, in excellent agreement with the theory." </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">"We believe our analysis pioneers interstellar <font style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" color="blue"><span style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" class="kLink">chemistry</span></font> studies at high redshift and demonstrates that it is possible, together with the detection of other molecules such as HD or CH, to use interstellar chemistry to tackle important cosmological issues," adds Srianand. </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">The results described here have been presented in a Letter to the Editor in Astronomy and Astrophysics ("First detection of CO in a high-redshift damped Lyman-alpha system", by R. Srianand et al.). </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">Notes </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">[1]: The team is composed of Raghunathan Srianand (IUCAA, Pune, India), Pasquier Noterdaeme and Cedric Ledoux (ESO), and Patrick Petitjean (IAP, France). The same team already made the first measurement of the temperature of the cosmic microwave background radiation, at a time when the Universe was only about 2.5 billion years old, also using UVES on the VLT (see ESO 27/00). At that time, they could only measure a temperature in the range between 6 and 14 K. </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">[2]: Quasars are extraordinarily luminous objects in the distant Universe, thought to be powered by supermassive black holes at the heart of galaxies. A single quasar could be a thousand times brighter than an entire galaxy of a hundred billion stars, and yet this remarkable amount of energy originates from a volume smaller than our Solar System. </font></p> <p align="left"> <font face="geneva,arial,verdana" size="-1">[3]: One of the fundamental predictions of the Hot <font style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" color="blue"><span style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" class="kLink">Big </span><span style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" class="kLink">Bang</span></font> theory for the creation of the Universe is the existence of the Cosmic Microwave Background Radiation (CMBR). This relic radiation of the primeval fireball was discovered in 1964 by means of radio observations by American physicists Arno A. Penzias and Robert W. Wilson, who were rewarded with the Nobel Prize in 1978. Precision measurements by the COBE and WMAP satellites later showed that this ancient <font style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" color="blue"><span style="color:blue!important;font-family:geneva,arial,verdana;font-weight:400;font-size:13px" class="kLink">radiation</span></font> fills the Universe, with a present-day temperature of slightly less than 3 degrees above absolute zero (2.725 Kelvin, or -270.4 degree Celsius). A particular prediction of the Big Bang theory is that the Universe cools when expanding, the temperature scaling with the dilution factor of the Universe (1 + redshift). At the redshift of the galaxy (2.41837), one would thus expect a temperature of 2.725 x (1 + 2.41837) = 9.315 K or -263.835 degree Celsius. </font></p><p align="left">&nbsp;</p><p align="left">&nbsp;</p><p align="left"><font size="4"><strong>And here's the actual news-item from the paper (red *):</strong></font></p><p align="left"><br /> <img src="http://sitelife.space.com/ver1.0/Content/images/store/10/8/aafec68a-87ff-4c4e-a871-f66f1ac3e731.Medium.png" alt="" /><br /><br /><br />Fig. 5. Measurements of T (CMBR) at various z. The star with errorbars is for the measurement based on CO presented here. Our earlier measurement using fine-structure lines of neutral carbon, 6.0 < TCMBR < 14.0 K, at z =2.33771 is indicated by the long vertical bar (Srianand et al. 2000).Measurement byMolaro et al. (2002) is marked by an open circle. Upper limits are measurements using C i or C ii &lowast; from the literature (squares) and using C i from our UVES sample (hexagons). The dashed line is the prediction from the hot big-bang theory, CMBR(z)=TCMBR(z = 0) &times; (1 + z). TCMBR measurement at z = 0 is based on the COBE determination (Mather et al. 1999). </p><p align="left">&nbsp;</p><p align="left">&nbsp;</p><p align="left"><font size="2"><strong>They measured the temperature of 11 Gy old CMB by using distant galaxy's interstellar CO as a proxy. Amazing work. Rock on ESO!&nbsp;</strong></font></p><p align="left">&nbsp;</p> <div class="Discussion_UserSignature"> </div>
 
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