Radio Spectra of the RATAN-600 RZF Radio Spectra of the RATAN-600 RZF objects and population analysis objects and population analysis

of weak radio sourcesof weak radio sourcesSemenova T.A., Parijskij Yu.N., Bursov N.N.Semenova T.A., Parijskij Yu.N., Bursov N.N.

SAO RASSAO RAS

We considered the next questions:We considered the next questions: RZF (RATAN-600 Zenith Field) catalog

RZF and all-z luminosity range

Type of spectra of RZF catalog

RZF, FIRST and SDSS objects

Multi-band photometry

RZF and all-z Luminosity RangeRZF and all-z Luminosity Range

RZF High Radio Luminosity box

VLA Deep Fields

GB 5GHz Sky

The modern luminosity The modern luminosity function of radio function of radio sources of the surveys sources of the surveys VLA deep fields, VLA deep fields, RATAN-600 and GB RATAN-600 and GB 5GHz. 5GHz. The RZF survey is The RZF survey is intermediate, with is intermediate, with is depth sufficient for the depth sufficient for the study of the whole part study of the whole part of the luminosity of the luminosity function connected with function connected with radio galaxiesradio galaxies..

RZF (Ratan-600 Zenith Field) catalogRZF (Ratan-600 Zenith Field) catalog

The catalog is a part of the deep multi-frequency survey of The catalog is a part of the deep multi-frequency survey of the sky with RATAN-600 near the local zenith in a strip the sky with RATAN-600 near the local zenith in a strip 00hh <RA<24h, at DECLINATION =DEC 3C84 <RA<24h, at DECLINATION =DEC 3C84 ++//--2 arcmin.2 arcmin.This catalog is resulted within the context of “Cosmological This catalog is resulted within the context of “Cosmological Gene” project (http://www.sao.ru/hg/CG/CG.html)Gene” project (http://www.sao.ru/hg/CG/CG.html)

Type of spectraType of spectra

Normal (-1.1<Normal (-1.1<α α ≤-0.5 ) 54.0%≤-0.5 ) 54.0% Flat (-0.5<Flat (-0.5<αα≤0) 25.8%≤0) 25.8%

Inverted (0<Inverted (0<α α ≤2.5 ) 6%≤2.5 ) 6%

Ultra Steep (-1.1 ≤ Ultra Steep (-1.1 ≤ α α <-2.0) 15.2%<-2.0) 15.2%

Comparison of histograms of distribution of spectral indexes of strong radio sources (empty rectangles) and faint radio sources (filled rectangles, from data of the RZF catalog).

The histogram of a difference of distribution of spectral indexes of sources of surveys on RATAN-600а) Strong (NCP> 200mJy)б) Weak (RZF survey <20mJy)

The full number of objects was identical

RZF objects with inverted spectraRZF objects with inverted spectra(~1% of RZF objects)(~1% of RZF objects)

First attempt to estimate Spectra of the First attempt to estimate Spectra of the WEAKEST population of NVSS SkyWEAKEST population of NVSS Sky

From of 10299 NVSS objects we divided into types:

MOST objects have NORMAL spectraUSS population- 15%Inverted spectra- 5%

Identification of RZF objects of the FIRST catalog Identification of RZF objects of the FIRST catalog resulted in the following statisticsresulted in the following statistics

Empty fieldsEmpty fields 5% 5%

Quasi-pointlike radio sources Quasi-pointlike radio sources ((LASLAS<6 <6 arc secarc sec)) 65%65%

Binary radio galaxies and quasars Binary radio galaxies and quasars 13%13%

Triple objects Triple objects 2%2%

Multiple objectsMultiple objects 9% 9%

Traces of “wind” in clustersTraces of “wind” in clusters 3% 3%

Peculiar objectsPeculiar objects 3%3%

Sources IdentificationsSources IdentificationsMost of the sources were identified with NVSS and FIRST Most of the sources were identified with NVSS and FIRST

catalogs, but only 75% with SDSS.catalogs, but only 75% with SDSS.

Analysis of morphology of objects at the mJy level led to the Analysis of morphology of objects at the mJy level led to the following conclusions:following conclusions:

The “point-like” population prevails (this is caused by too The “point-like” population prevails (this is caused by too large red shifts Z for powerful radio galaxies and by large red shifts Z for powerful radio galaxies and by transition to objects of small radio luminosity of the type transition to objects of small radio luminosity of the type AGN, Star-Burst galaxies). By “point-like” sources we mean AGN, Star-Burst galaxies). By “point-like” sources we mean objects that were not resolved by the catalog FIRST with its objects that were not resolved by the catalog FIRST with its 6” diagram.6” diagram.

SDSS data often show sings of a possible gravitational SDSS data often show sings of a possible gravitational disturbance of a host galaxy by a neighbor object. disturbance of a host galaxy by a neighbor object.

Example of possible gravitational disturbances of a host Example of possible gravitational disturbances of a host galaxy by a neighbor object – the influence of close galaxy by a neighbor object – the influence of close galaxies on generation of powerful radio emission galaxies on generation of powerful radio emission

An example of a binary FRII type radio galaxy in the An example of a binary FRII type radio galaxy in the RZF survey band by data of the RZF, FIRST RZF survey band by data of the RZF, FIRST

and SDSS catalogsand SDSS catalogs

An example of an unusual object of the “FRII binary” An example of an unusual object of the “FRII binary” type by data of the RZF, FIRST and SDSS catalogstype by data of the RZF, FIRST and SDSS catalogs

Multi-band photometryMulti-band photometry About 20% of the RZF sources are beyond r=22.5 and should have About 20% of the RZF sources are beyond r=22.5 and should have

z>1z>1

Using the “Large Trio” experience, we found color red shifts for Using the “Large Trio” experience, we found color red shifts for extremely faint SDSS objects.extremely faint SDSS objects.

Attempts of finding traces of “Break-galaxies” with the cut of Attempts of finding traces of “Break-galaxies” with the cut of optical emission beyond 912A by the SDSS filters u3540A, optical emission beyond 912A by the SDSS filters u3540A, g4925A, r6335A, i7800A, z9294A gave a list of candidates to g4925A, r6335A, i7800A, z9294A gave a list of candidates to distant objects (Break-galaxies)distant objects (Break-galaxies)

z~4.5 z~4.5 19 objects (g-r>2m)19 objects (g-r>2m)z~6z~6 4 objects (r-i>2m) 4 objects (r-i>2m)z~7z~7 3 objects (i-r>2m) 3 objects (i-r>2m)

The getting of the powerful Ly-alpha line into a filter causes an The getting of the powerful Ly-alpha line into a filter causes an increase of brightness in this filter over neighbor filters for the increase of brightness in this filter over neighbor filters for the population of powerful galaxies which are strong emitters in the population of powerful galaxies which are strong emitters in the Ly-alpha line (the experiment of the “Large Trio” in RC Ly-alpha line (the experiment of the “Large Trio” in RC J0105+05). Analysis of obtained data resulted in detection of 3 J0105+05). Analysis of obtained data resulted in detection of 3 analogous cases of the getting in the R filter (Z~4.2) and 3 cases analogous cases of the getting in the R filter (Z~4.2) and 3 cases in the I filter (Z~5.4).in the I filter (Z~5.4).

ConclusionsConclusions

Most of the sources were identified with NVSS and Most of the sources were identified with NVSS and FIRST catalogs, but only 75% with SDSS objects. FIRST catalogs, but only 75% with SDSS objects.

Multi-band photometry of SDSS data showed that Multi-band photometry of SDSS data showed that 20% of host galaxies are fainter than r=22.5m and they can 20% of host galaxies are fainter than r=22.5m and they can have large red shifts (z>1).have large red shifts (z>1).

The population of FRII objects is presented worse in The population of FRII objects is presented worse in the RZF catalog than in catalogs with higher extreme the RZF catalog than in catalogs with higher extreme fluxes. Observation confirmed a sharp fall of percentage of fluxes. Observation confirmed a sharp fall of percentage of FRII objects. This does not contradict to recent models.FRII objects. This does not contradict to recent models.

This is usually interpreted as the change of a relative role of This is usually interpreted as the change of a relative role of populations of objects with steep, flat and inverse spectra. populations of objects with steep, flat and inverse spectra.

Thank you for your attention Thank you for your attention

λ f0 Δf ΔT Входной усилитель Ta Tс

cm GHz GHz Tph, K Ttype Tn,K K K

1.4 21.7 2.5 3.5 15 HEMT 23 30 77

2.7 11.2 1.4 3 15 HEMT 12 25 65

3.9 7.7 1.0 3 15 HEMT 14 23 62

6.3 4.8 0.9 2.2 15 HEMT 6 22 39

13.0 2.3 0.4 8 310 HEMT 35 25 95

31.0 0.96 0.12 15 310 HEMT 21 50 105

49.5 0.61 0.128 25 310 HEMT 25 70 125

где λ и f0 - длина волны и центральная частота,Δf   - полоса частот, ΔT - чувствительность при постоянной времени 1 сек,Тф и Tш - физическая и шумовая температуры входных усилителей и их

типы: HEMT  - транзистор с высокой подвижностью электронов, Та

*    - температура антенны на средних углах возвышения, Та

**   - шумовая температура антенны в зените, Тс       - общая шумовая температура системы.