Atomic gas (HI) in Isolated Galaxies Daniel Espada Fernández Advisor: Lourdes Verdes-Montenegro...

Atomic gas (HI) in Atomic gas (HI) in Isolated Galaxies Isolated Galaxies

Daniel Espada Fernández Daniel Espada Fernández Advisor: Lourdes Verdes-MontenegroAdvisor: Lourdes Verdes-MontenegroDpto. de Astronomía ExtragalácticaDpto. de Astronomía Extragaláctica

IAA-CSICIAA-CSIC

Overview Overview

3- HI study of isolated galaxies3- HI study of isolated galaxies

2- The sample of isolated galaxies2- The sample of isolated galaxies

4- Work in the future4- Work in the future

1- Introduction to the AMIGA project1- Introduction to the AMIGA project

TeamTeam

AYA 2002-03338

Instituto de Astrofísica de AndalucíaInstituto de Astrofísica de Andalucía

Emilio García Emilio García (System Manager)(System Manager) Stéphane Leon Stéphane Leon (PostDoc)(PostDoc) Ute Lisenfeld Ute Lisenfeld (PostDoc)(PostDoc) Lourdes Verdes-Montenegro Lourdes Verdes-Montenegro (Staff, (Staff,

P.I.)P.I.) José Sabater José Sabater (PhD candidate)(PhD candidate) Simon Verley Simon Verley (PhD candidate, IAA – (PhD candidate, IAA –

Obs. Paris) Obs. Paris) Daniel Espada Daniel Espada (PhD candidate)(PhD candidate)

International collaborationInternational collaboration

Jack Sulentic –Jack Sulentic – University of University of AlabamaAlabama

Steve Odewahn –Steve Odewahn – Arizona State Arizona State UniversityUniversity

Walter Huchtmeier –Walter Huchtmeier – Max Planck Max Planck Institute of BonnInstitute of Bonn

Min S. Yun –Min S. Yun – FCRAO FCRAO Soledad del Rio – Soledad del Rio – INAOEINAOE

TeamTeam

Instituto de Astrofísica de AndalucíaInstituto de Astrofísica de Andalucía

Emilio García Emilio García (System Manager)(System Manager) Stéphane Leon Stéphane Leon (PostDoc)(PostDoc) Ute Lisenfeld Ute Lisenfeld (PostDoc)(PostDoc) Lourdes Verdes-Montenegro Lourdes Verdes-Montenegro (Staff, (Staff,

P.I.)P.I.) José Sabater José Sabater (PhD candidate)(PhD candidate) Simon Verley Simon Verley (PhD candidate, IAA – (PhD candidate, IAA –

Obs. Paris) Obs. Paris) Daniel Espada Daniel Espada (PhD candidate)(PhD candidate)

International collaborationInternational collaboration

Jack Sulentic –Jack Sulentic – University of Alabama University of Alabama Steve Odewahn –Steve Odewahn – Arizona State Arizona State

UniversityUniversity Walter Huchtmeier –Walter Huchtmeier – Max Planck Max Planck

Institute of BonnInstitute of Bonn Min S. Yun –Min S. Yun – FCRAO FCRAO Soledad del Rio – Soledad del Rio – INAOEINAOE

Françoise Combes –Françoise Combes – Paris Paris ObservatoryObservatory

Margarita Rosado –Margarita Rosado – UNAM UNAM A. Bosma, L. Athanassoula (Obs.

Marseille) M. Gutiérrez-Valdez (Univ.

Guanajuato) I. Puerari (INAOE) A. Ballu (ENSP Strasbourg)

AYA 2002-03338

1.Introduction of the AMIGA project1.Introduction of the AMIGA project

-Motivation:-Motivation: Role of the environment in the formation and evolution of galaxiesRole of the environment in the formation and evolution of galaxies reference sample with minimum influence from the environmentreference sample with minimum influence from the environment properties of ISM as a function of isolation, and its relation to properties of ISM as a function of isolation, and its relation to

morphology, luminosities, star formation and nuclear activity.morphology, luminosities, star formation and nuclear activity.

-Multifrequency study:-Multifrequency study: optical, FIR, NIR, Ha, CO, radiocontinuum, HIoptical, FIR, NIR, Ha, CO, radiocontinuum, HI

-Reference of isolated galaxies needed:-Reference of isolated galaxies needed: Catalogue of isolated galaxies (CIG, Karachentseva 1973)Catalogue of isolated galaxies (CIG, Karachentseva 1973)

http://www.iaa.es/AMIGA.htmlhttp://www.iaa.es/AMIGA.html

Isolation criterion (Karachentseva, 1973): Isolation criterion (Karachentseva, 1973): A galaxy (diameter=d) is isolated if there isn’t any other galaxy (d’):A galaxy (diameter=d) is isolated if there isn’t any other galaxy (d’):

¼ d < d’ < 4 d¼ d < d’ < 4 d Angular separation < 20 d’Angular separation < 20 d’

POSS-I platesPOSS-I plates Northern hemisphere: dec > -3ºNorthern hemisphere: dec > -3º Optical magnitude: down to 15.7 (B band)Optical magnitude: down to 15.7 (B band)

1051 isolated galaxies1051 isolated galaxies

Revision (1980):Revision (1980): 0 – Isolated (893)0 – Isolated (893) 1 – Marginally isolated (85)1 – Marginally isolated (85) 2 – Member of a group or a cluster 2 – Member of a group or a cluster

(64)(64)

2. The sample of isolated galaxies2. The sample of isolated galaxies

b) b) Blue luminosityBlue luminosity: large : large range of luminosities;range of luminosities;

a) a) VelocityVelocity: the CIG : the CIG samples a deep enough samples a deep enough volume of space to volume of space to measure the radio, IR and measure the radio, IR and optical luminosity optical luminosity functions;functions;

c) c) MorphologyMorphology: the CIG is : the CIG is morphologically diverse to morphologically diverse to permit statistical studies permit statistical studies correlated with Hubble correlated with Hubble type.type.

2. The sample of isolated galaxies2. The sample of isolated galaxies

3. HI study of isolated galaxies3. HI study of isolated galaxies

IntroductionIntroduction -hiperfine transition of H, -hiperfine transition of H, λλ=21cm=21cm-provides information about : -content of atomic gas-provides information about : -content of atomic gas -kinematics-kinematics -tracer of interactions-tracer of interactions

3.1-HI content3.1-HI content

3.2-HI profile asymmetries3.2-HI profile asymmetries

Objectives:

3.1 -HI content3.1 -HI content

DENSER ENVIRONMENTDENSER ENVIRONMENT: spirals in clusters are HI : spirals in clusters are HI deficients (Van Gorkom et al 1996) and some of them are deficients (Van Gorkom et al 1996) and some of them are stripped until 90% of their HI (Haynes et al 1990). stripped until 90% of their HI (Haynes et al 1990).

-> -> HI DEFICIENCY CAUSED BY INTERACTIONHI DEFICIENCY CAUSED BY INTERACTION REFERENCES OF ISOLATED GALAXIESREFERENCES OF ISOLATED GALAXIES: Until now the : Until now the

best reference was Haynes et al 1984 = 324 isolated best reference was Haynes et al 1984 = 324 isolated galaxies observed in HI; or field galaxies.galaxies observed in HI; or field galaxies.

3.Atomic gas

1. LITERATURE

2. IMPROVEMENTS OF OUR STUDY OF IG

Quantity: -Doubles the number of gal. (lower dispersion in subsamples)Quality: -Exhaustive bibliographic compilation -Selection of the best profiles (extent/beam) -repeat not satisfactory observations

-100 articles-100 articles-365 galaxies were already observed, selection of data, -365 galaxies were already observed, selection of data,

digitalization of profilesdigitalization of profiles

4. COMPILATION OF DATA

5. OBSERVATIONS


3.Atomic gas



Effelsberg 100m, Germany. 155


5. OBSERVATIONS


3.Atomic gas



GBT 100x110m, Green Bank,MA, USA 51



5. OBSERVATIONS


3.Atomic gas



NRT, Nançay ,France 129



4.COMPILATION OF DATA

5. OBSERVATIONS


3.Atomic gas



Arecibo 304m, Puerto Rico 34

NRT, Nançay ,France 129




5. OBSERVATIONS


3.Atomic gas

GBT

POSSI

Radial velocity : 3341 +/- 9 km/sDiameters: 1.3 x 0.9 arcmin Magnitude : 15.1 Type: Sm

Flux HI=S=6.05 +- 0.11 Jy km/s Width=220 km/svelocity HI= 3336+-10 km/s

3.Atomic gas

6. HI PROFILE EXAMPLE: CIG 661

90% of the IG observed + 200 hours at Nancay.90% of the IG observed + 200 hours at Nancay. 100% profiles calibrated & reduced for the IG 100% profiles calibrated & reduced for the IG

observed, but not corrected for beam attenuationobserved, but not corrected for beam attenuation Data available in the DB for the study:Data available in the DB for the study:

3.1.HI content3.1.HI content 7. STATUS

3.Atomic gas

S= integrated flux

D25 d25 = diameters (= Ø)

B = beam of the telescope

LB = Blue luminosity

M(HI) = f(LB, Ø, t)

t= type

Sc = Sc(D25,d25, B, t) = beam/extent corrected int. flux

MHI= 2.36 105 D2 [Mpc] Sc[Jy km/s]

D = distance

3.2.HI-profile asymmetry3.2.HI-profile asymmetry

a) OTHER SAMPLES OF ISOLATED GALAXIESa) OTHER SAMPLES OF ISOLATED GALAXIES

N=104 Haynes et al 1998N=104 Haynes et al 1998N=30 Matthews et al 1998 N=30 Matthews et al 1998

b) OTHER ENVIRONMENTS b) OTHER ENVIRONMENTS -Clusters -Clusters N=30 Sp Van Driel et al 1998 77%N=30 Sp Van Driel et al 1998 77%N=1700 Richter & Sancisi 1994 50 % N=1700 Richter & Sancisi 1994 50 % (Visual examination)(Visual examination)-Groups-GroupsN=100 Sulentic & Arp 1983 most of asymmetric prof. areN=100 Sulentic & Arp 1983 most of asymmetric prof. are

not isolated galaxies not isolated galaxies

50 % of them have asymmetric profiles!

3.Atomic gas

1. LITERATURE

3.2.HI-profile asymmetry3.2.HI-profile asymmetry 3.Atomic gas

2. ASYMMETRY CALCULATIONS

F1 F2

F1

F2

A=

vm

V

F

• Example of asymmetry coefficient:

•Examples of real HI profiles: CIG421(asymmetric) & CIG736 (symmetric)

A=1.13 A=1.01


-N=40 isolated galaxies observed by us -S/N>10

-Around 50 % of them have asymmetric profilesas in previous studies (but N is small and not reliable…)

3.Atomic gas

• First results:


1) Pointing offsets of the radiotelescope.1) Pointing offsets of the radiotelescope.

2) Confusion with companions within the radiotelescope 2) Confusion with companions within the radiotelescope beam.beam.

3) Noncircular motions. 3) Noncircular motions.

4) True distortions in the HI mass distribution4) True distortions in the HI mass distribution..

3.Atomic gas

3. EXPLANATIONS FOR LOPSIDENESS

-Asymmetries in IG are caused by small HI-rich companions or are intrinsic to the isolated galaxy???.

HI MAPS needed

3.2.HI-profile asymmetry3.2.HI-profile asymmetry 4. “HI MAPS of IG” LITERATURE

-D. J. Pisano ’s Thesis 2001, 41 “isolated galaxies” observed at VLA and ATCA to observe HI clouds down to MHI=10^7 13 of them had HI-rich companions… BUT -the isolation criteria wasn’t so restrictive as our -galaxies without z wasn’t taken into account

3.Atomic gas

Observations at the VLA (proposed for the next season). Subsample: 10, with A>1.10, S/N>10, very isolated and beam/extent>2

3.2.HI-profile asymmetry3.2.HI-profile asymmetry 4. “HI MAPS of IG” LITERATURE

-D. J. Pisano ’s Thesis 2001, 41 “isolated galaxies” observed at VLA and ATCA to observe HI clouds down to MHI=10^7 13 of them had HI-rich companions… BUT -the isolation criteria wasn’t so restrictive as our -galaxies without z wasn’t taken into account

3.Atomic gas

4.Work in the future4.Work in the future

Comparison with samples of galaxies in denser Comparison with samples of galaxies in denser environments (groups).environments (groups).

Correlation with other comp. of the ISM and SF. Correlation with other comp. of the ISM and SF.

Ex: MHI+H2 vs SFEx: MHI+H2 vs SF HI content vs bars, AGNs.HI content vs bars, AGNs. Studies for a subsample of very isolated HI-rich Studies for a subsample of very isolated HI-rich

galaxies with 2D-information (VLA).galaxies with 2D-information (VLA).

• Collaboration with SubMillimiter Array (SMA) in the calibration of the interferometer, using CIG galaxies.

FINFIN

C.Public database C.Public database

Vatican Observatory Summer School 2003Vatican Observatory Summer School 2003

Status of the projectStatus of the project

•Isolation criteria:77 % of the POSS fields checked Isolation criteria:77 % of the POSS fields checked

•LLBB y L y LFIRFIR for the whole sample for the whole sample

•36 % H36 % H of the subsample observed of the subsample observed

•67 % CO of the subsample observed or compiled67 % CO of the subsample observed or compiled

•85 % HI data has been observed or compiled85 % HI data has been observed or compiled

•80 % radio continuum reprocessed80 % radio continuum reprocessed

IAA-CSIC, GranadaEffelsberg 100m, Bonn,Germ.

Arecibo 304m, PuertoRico

FCRAO 14m, Mass., USA

IRAM 30m, GranadaSpain

Nançay,France

Atomic gas (HI) in Isolated Galaxies Daniel Espada Fernández Advisor: Lourdes Verdes-Montenegro...

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