Measuring the Density and Temperature of Starburst Galaxies

TIP Last Changed: JeffMangum - 25 May 2010

Table of Contents:

Student's To Do List

  1. Read background information on molecular excitation, star formation, formaldehyde, ammonia, etc.
  2. Introduction to data analysis (AIPS and CLASS) and first look at data to be analyzed.
  3. Step through analysis tasks:
    1. GBTIDL or CLASS:
      • Determine best spectral smoothing to apply to all spectra.
      • Fit baselines to all spectra.
      • Find best gaussian fits to all spectra. May involve fitting multiple (overlapping) gaussians which are comprised of both emission and absorption components.
      • Tabulate gaussian fit results, which should include at least the following for each gaussian:
        • Peak intensity (in K)
        • Central velocity (in km/s)
        • FWHM (in km/s)
        • Integrated intensity (in K*km/s)
    2. CASA or AIPS:
      • Data editing and calibration
      • Imaging
      • Analysis (line parameter measurements from gaussian fits, etc.)
  4. Compare derived gaussian fit parameters from each H2CO and/or NH3 transition for similar velocity components within each source. FWHM and central velocity should be very similar.
  5. Form H2CO and NH3 transition ratios for each source/velocity component integrated intensities using proper statistics. Be sure to apply appropriate Ta-to-Tmb calibration factors. Check out my analysis of the amplitude calibration measurements in ExgalFormaldehyde and ExgalAmmoniaGBT.
  6. Study use of line ratios to derive physical conditions. Apply to H2CO and NH3 measurements using the specific physical structure of the H2CO and NH3 molecules to this problem.
  7. Analyze dependence of line ratio on density, temperature, and abundance to understand limitations of line ratio measurements for deriving physical conditions (specifically, density) in star formation regions. Use radiative transfer model (LVG and/or Monte Carlo) in this investigation.
  8. Apply all of the above to the derivation of the spatial density and kinetic temperature in starburst galaxy sample.
  9. Put derived physical conditions within the context of other measurements of physical conditions in each starburst galaxy. This will allow for an improved understanding of the physical structure of each starburst galaxy.

Background

The Physical Conditions Within Starburst Galaxies

Studies of the distribution of Carbon Monoxide (CO) emission in external galaxies (cf. Young & Scoville (1991)) have pointed to the presence of large quantities of molecular material in these systems. These studies have yielded a detailed picture of the molecular mass in many external galaxies. But, because emission from the abundant CO molecule is generally dominated by radiative transfer effects, such as high optical depth, it is not a reliable monitor of the physical conditions, such as spatial density and kinetic temperature, quantities necessary to assess the possibility of star formation. Emission from less-abundant, higher-dipole moment molecules are better-suited to the task of deriving the spatial density and kinetic temperature of the dense gas in our and external galaxies. For this reason, emission line studies from a variety of molecules have been made toward mainly nearby galaxies (see Mauersberger & Henkel (1989) (CS), Gao & Solomon (2004a) (HCN), Nguyen-Q-Rieu et al. (1992) (HCO+), Mauersberger et al. (1990) and Meier & Turner (2005) (HC3N), Mauersberger et al. (2003) (NH3), or Henkel, Baan, & Mauersberger (1991) for a review). The most extensive sets of measurements of molecular line emission in external galaxies has been done using the J=1-0 transitions of CO (Helfer et al. 2003) and HCN (Gao & Solomon 2004a). Since the J=1-0 transitions of CO and HCN are good tracers of the more generally distributed and the denser gas, respectively, but do not provide comprehensive information about the individual physical conditions of the dense, potentially star-forming gas, another molecule must be observed for this purpose.

Density Measurement Using Formaldehyde

Formaldehyde (H2CO) has proven to be a reliable density and kinetic temperature probe in Galactic molecular clouds. Existing measurements of the H2CO 1(10)-1(11) and 2(11)-2(12) emission in a wide variety of galaxies by Baan et al. (1986), Baan et al. (1990), Baan et al. (1993), and Araya et al. (2004) have mainly concentrated on measurements of the 1(10)-1(11) transition. One of our goals with the present study was to obtain a uniform set of measurements of both K-doublet transitions with which the physical conditions, specifically the spatial density, in the extragalactic context could be derived. Using the unique density selectivity of the K-doublet transitions of H2CO we have measured the spatial density in a sample of galaxies exhibiting starburst phenomena and/or high infrared luminosity.

Results from the first phase of this work, which was a "pilot survey" of a sample of mainly nearby galaxies measured using the GBT (Mangum et al . (2008) has shown that H2CO is a reliable and accurate density probe for extragalactic environments where the kinetic temperature is known. See our recent poster describing this work presented at the Infrared Emission, ISM and Star Formation workshop held at MPIA in Heidelberg, Germany, February 22-24.

FormaldehydeDensitometryStarburstPosterIR10.jpg
Formaldehyde Densitometry of Starburst Galaxies poster presentation given at the 'IR10' conference.

This then leads us to the second part of this project...

Kinetic Temperature Measurement Using Ammonia

The derivation of n(H2) in our sample of starburst galaxies currently relies upon assumed kinetic temperatures. The inversion transitions of NH3 and the rotational transitions of H2CO possess very similar excitation conditions, thus likely trace similar dense gas environments. Using the unique sensitivities to kinetic temperature afforded by the excitation characteristics of several inversion transitions of NH3 , we can continue our characterization of the dense gas in galaxies exhibiting starbursts by measuring the kinetic temperature in a sample of galaxies selected for their high infrared luminosity. This extension of our successful galaxy survey will allow us to further study the range of mean physical conditions which give rise to star formation in some of the most starburst-active galaxies known.

Formaldehyde as a Spatial Density Probe

Formaldehyde is a proven tracer of the high density environs of molecular clouds. It is ubiquitous: H2CO is associated with 80% of the HII regions surveyed by Downes et al. (1980), and possesses a large number of observationally accessible transitions from centimeter to far-infrared wavelengths. Because H2 CO is a slightly asymmetric rotor molecule, most rotational energy levels are split by this asymmetry into two energy levels. Therefore, the energy levels must be designated by a total angular momentum quantum number, J, the projection of J along the symmetry axis for a limiting prolate symmetric top, K-1 , and the projection of J along the symmetry axis for a limiting oblate symmetric top, K+1 . This splitting leads to two basic types of transitions: the high-frequency ∆J = 1, ∆K−1 = 0, K+1 = −1 “P-branch” transitions and the lower-frequency ∆J = 0, ∆K−1 = 0, ∆K+1 = ±1 “Q-branch” transitions, popularly known as the "K-doublet” transitions (see discussion in Mangum & Wootten (1993)). The P-branch transitions are only seen in emission in regions where n(H2 ) >= 10^4 cm−3 . The excitation of the K-doublet transitions, though, is not so simple. For n(H2 ) < 10^5.5 cm−3 , the lower energy states of the 1(10)−1(11) through 5(14)−5(15) K-doublet transitions become overpopulated due to a collisional selection effect (Evans et al. (1975); Garrison et al. (1975)). This overpopulation cools the J ≤ 5 K-doublets to excitation temperatures lower than that of the cosmic microwave background, causing them to appear in absorption. For n(H2 ) > 10^5.5 cm−3 , this collisional pump is quenched and the J ≤ 5 K-doublets are then seen in emission over a wide range of kinetic temperatures and abundances (see Figure 1 in Mangum etal (2008)).

Ammonia as a Kinetic Temperature Probe

Ammonia is a proven and unbiased tracer of the high density regions within molecular clouds in a variety of galactic and extragalactic environments (cf. Walmsley & Ungerechts (1983), Mauersberger et al . (2003)). Because NH3 is a symmetric top molecule (energy levels given by quantum numbers (J,K)), exchange of population between the K-ladders within a given symmetry state (ortho or para) occurs only via collisional processes. The relative intensity of these rotational energy levels then represents the urgently needed direct measure of the kinetic temperature (cf. Figure 1), breaking the Tk – n(H2 ) degeneracy. The inversion transitions of NH3 at 23–27 GHz have been used to monitor the kinetic temperature in both cool (TK ≃ 20 K) and warm (TK ≃ 300 K) galactic and extragalactic star formation environments. For example, a study of the NH3 (1,1) through (9,9) transitions toward NGC 253, IC 342, and Maffei 2 by Mauersberger et al . (2003) revealed warm (TK = 100–140 K) gas toward NGC 253, IC 342, and Maffei 2 and cooler gas (TK = 60 K) toward M82. In this study, the NH3 (2,2)/(1,1) line ratio monitors lower kinetic temperatures (<= 40 K), while the NH3 (4,4)/(2,2) ratio monitors the higher kinetic temperatures (<= 150 K) in our starburst galaxy sample.

The Big Picture

Ultimately, we want to know how galaxies evolve. The density and temperature measurements conducted with this work is a major step in this direction, as it will ultimately allow us to determine the density and temperature evolution of galaxies from the Milky Way to the edges of the universe.

Reference Material

Observations To Be Analyzed

Very Large Array (VLA)

The VLA was used to image the H2CO 1(10)-1(11) and 2(11)-2(12) emission in NGC253, M83, and IC342. This project represents a follow-up to our GBT survey of H2CO emission in these and other starburst galaxies, with a goal towards identifying the spatial structure of the dense gas in these starburst galaxies. These 1.2 arcsec spatial resolution measurements should allow for a very clear characterization of the dense gas structure in these classic starburst galaxies. Reduction and analysis of these measurements has been patiently waiting for a dedicated student to carry the project forward!

Green Bank Telescope (GBT)

Formaldehyde Measurements

The Green Bank Telescope (GBT) has been used to make single-pointing measurements of the 1(10)-1(11) (4.8 GHz) and 2(11)-2(12) GHz) K-doublet transitions of H2CO toward a sample of 52 galaxies exhibiting various aspects of starburst activity. The first phase of this project was published in Mangum etal. (2008). A follow-up paper, which adds to the data presented in our 2008 paper, is currently being analyzed. Some of the measurements of the H2CO emission and absorption in the 1(10)-1(11) and 2(11)-2(12) transitions toward our starburst galaxy sample are shown in the following figures.

ExgalFormSingles-page1.jpg
H2CO 1(10)-1(11) and 2(11)-2(12) measurements in starburst galaxies.
ExgalFormSingles-page2.jpg
H2CO 1(10)-1(11) and 2(11)-2(12) measurements in starburst galaxies (cotinued).

NGC253FormSpec.jpg
NGC253
Mrk231FormSpec.jpg
Mrk231
IC342FormSpec.jpg
IC342
M82FormSpec.jpg
M82
NGC3079FormSpec.jpg
NGC3079

NGC3628FormSpec.jpg
NGC3628
IC860FormSpec.jpg
IC860
M83FormSpec.jpg
M83
IR15107FormSpec.jpg
IR15107
Arp220FormSpec.jpg
Arp220
NGC6946FormSpec.jpg
NGC6946

NGC2146FormSpec.jpg
NGC2146
NGC2903FormSpec.jpg
NGC2903

Ammonia Measurements

The Green Bank Telescope (GBT) has been used to make single-pointing measurements of the (1,1), (2,2), and (4,4) transitions transitions of NH3 near 24 GHz toward starburst galaxies where we have detected H2CO. The major portion of this project is currently scheduled on the GBT and is in-progress. A sample of NH3 (1,1), (2,2), and (4,4) measurements toward three starburst galaxies is shown in the following figures.

NGC253NH3.jpg
NGC253
IC342NH3.jpg
IC342
NGC6946NH3.jpg
NGC6946

-- JeffMangum - 2010-02-17
Topic revision: r9 - 2014-08-01, JeffMangum
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