How does the average SED of normal galaxies match with the CE01 template?

The average FIR SED of normal galaxies appears to match well with the CE01 template of similar luminosity, but that of cold galaxies is matched withroughly 80 times less luminous template, even if the median LIR of normal and cold galaxies are similar (〈LIR/L 〉 ∼ 5 × 1011 and 4 × 1011 L for normal and cold galaxies, respectively).

How many sources are in the IRAS Faint Sources Catalog?

The authors use the IRAS Faint Sources Catalog ver. 2 (Moshir, Kopman & Conrow 1992), which contains 173 044 sources with flux density measurements at 12, 25, 60 and 100 µm.

What is the reason for the low Tdust of SMGs?

This indicates that the low Tdust of SMGs could be caused by an overestimation of the FIR/(sub)millimetre fluxes due to blending problems.

How many SMGs are in the study?

Among them, the authors have three SMGs with Tdust measured in this study (Tdust for the other 10 galaxies are not measured because they did not fulfil the selection criteria in Section 2 due to the low signal-to-noise ratios in some bands), and show them as squares in Fig. 4(a).

How do the authors compute LIR for the local galaxies?

By adopting the same method applied to high-z galaxies, the authors compute LIR for the local galaxies by fitting the CE01 templates to the flux densities at λrest ≥ 30 µm.

What is the mean trend of Tdust for high-z galaxies?

This shows that Tdust is negative, on average, which indicates that Herschel-selected high-z LIRGs at 0.3 < z < 1.4 appear to be colder than AKARIselected local LIRGs.

What is the median trend of Tdust for Herschel-selected high-z?

Journal compilation C© 2010 RAS, MNRAS 409, 75–82we see that the median trend of Tdust for Herschel-selected high-z galaxies at z 0.5 becomes smaller than that for AKARI-selected low-z galaxies by 2–5 K at high luminosities (LIR > 5 × 1010 L ).

How do the authors compute LIR and Tdust for high-z galaxies?

For Tdust estimates, in addition to the conditions (i) and (ii) used for high-z galaxies, the authors use only sources detected at 140 or 160 µm.

How many galaxies are selected for the MBB model?

The authors then select galaxies having flux measurements on both sides of the peak for the best-fitting MBB model, and secure a final sample of 140 galaxies.

What is the median trend of Tdust for high-z galaxies?

In Fig. 4(a), the median trend of Tdust for high-z galaxies also appears fairly constant at low luminosities, but increases as LIR increases at higher luminosities.

What is the distribution of Tdust for high-z galaxies?

This shows that only ‘blended’galaxies have several cold galaxies with Tdust ∼ 20 K, while ‘clean’ galaxies do not (to be discussed in detail in Section 4.2).

(PDF) Evolution of Dust Temperature of Galaxies through Cosmic Time as seen by Herschel (2010) | Ho Seong Hwang

Most frequently asked questions

1. What are the contributions mentioned in the paper "Evolution of dust temperature of galaxies through cosmic time as seen by herschel" ?

The authors study the dust properties of galaxies in the redshift range 0. 1 z 2. 8 observed by the Herschel Space Observatory in the field of the Great Observatories Origins Deep Survey-North as part of the PACS Extragalactic Probe ( PEP ) and Herschel Multi-tiered Extragalactic Survey ( HerMES ) key programmes.. The authors show that this large dispersion of the LIR−Tdust relation can bridge the gap between local star-forming galaxies and high-z submillimetre galaxies ( SMGs ).. The authors also find that three SMGs with very low Tdust ( 20 K ) covered in this study have close neighbouring sources with similar 24-μm brightness, which could lead to an overestimation of FIR/ ( sub ) millimetre fluxes of the SMGs.

2. What is the SFE of the galaxies?

This SFE is known to be controlled by the gas density (Schmidt 1959; Kennicutt 1998),which is connected to the spatial extent of star-forming regions.

3. What is the mean Tdust scatter for high-z galaxies?

It is also seen that Tdust scatter increases by about 5 K in the sense that the upper envelope for high-z galaxies is similar to that of local galaxies, while the lower envelope for high-z galaxies stretches below.

4. How did the authors calculate uncertainty of LIR and Tdust?

Uncertainties of LIR and Tdust were computed by randomly selecting flux densities at each band within the associated error distribution (assumed to be Gaussian) and then refitting.

Evolution of Dust Temperature of Galaxies through Cosmic Time as seen by Herschel

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Most frequently asked questions

1. What are the contributions mentioned in the paper "Evolution of dust temperature of galaxies through cosmic time as seen by herschel" ?

2. What is the SFE of the galaxies?

3. What is the mean Tdust scatter for high-z galaxies?

4. How did the authors calculate uncertainty of LIR and Tdust?

5. How does the average SED of normal galaxies match with the CE01 template?

6. How many sources are in the IRAS Faint Sources Catalog?

7. What is the reason for the low Tdust of SMGs?

8. How many SMGs are in the study?

9. How do the authors compute LIR for the local galaxies?

10. What is the mean trend of Tdust for high-z galaxies?

11. What is the median trend of Tdust for Herschel-selected high-z?

12. How do the authors compute LIR and Tdust for high-z galaxies?

13. How many galaxies are selected for the MBB model?

14. What is the median trend of Tdust for high-z galaxies?

15. What is the distribution of Tdust for high-z galaxies?

Figures

Citations

GOODS–Herschel: an infrared main sequence for star-forming galaxies

PHIBSS: MOLECULAR GAS CONTENT AND SCALING RELATIONS IN z ∼ 1-3 MASSIVE, MAIN-SEQUENCE STAR-FORMING GALAXIES*

The Star Formation Mass Sequence Out to z = 2.5

The Herschel Multi-tiered Extragalactic Survey: HerMES

Modeling the Panchromatic Spectral Energy Distributions of Galaxies

References

The Seventh Data Release of the Sloan Digital Sky Survey

The Global Schmidt law in star forming galaxies

Classification parameters for the emission-line spectra of extragalactic objects

Herschel Space Observatory - An ESA facility for far-infrared and submillimetre astronomy

Herschel Space Observatory ? An ESA facility for far-infrared and submillimetre astronomy

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