Atomic hydrogen deficiency in spiral galaxies in clusters
We consider the new method for atomic hydrogen deficiency estimations. The main idea is to use the empirical relation between total HI mass and specific angular momentum of the disk for isolated galaxies. The method was compared with the standard one, based on dependence of HI mass on optical diamet...
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| Zitieren: | Atomic hydrogen deficiency in spiral galaxies in clusters / E.S. Shaldenkova // Advances in Astronomy and Space Physics. — 2011. — Т. 1., вип. 1-2. — С. 23-26. — Бібліогр.: 25 назв. — англ. |
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Digital Library of Periodicals of National Academy of Sciences of Ukraine| _version_ | 1859559479051288576 |
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| author | Shaldenkova, E.S. |
| author_facet | Shaldenkova, E.S. |
| citation_txt | Atomic hydrogen deficiency in spiral galaxies in clusters / E.S. Shaldenkova // Advances in Astronomy and Space Physics. — 2011. — Т. 1., вип. 1-2. — С. 23-26. — Бібліогр.: 25 назв. — англ. |
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| description | We consider the new method for atomic hydrogen deficiency estimations. The main idea is to use the empirical relation between total HI mass and specific angular momentum of the disk for isolated galaxies. The method was compared with the standard one, based on dependence of HI mass on optical diameter and galaxy type. They both were applied to Virgo and Coma cluster galaxies and to Local Volume galaxies. Also we investigated possible mechanisms responsible for HI deficiency in cluster spirals.
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| first_indexed | 2025-11-26T14:23:46Z |
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Atomic hydrogen de�ciency in spiral galaxies in clusters
E. S. Shaldenkova
Sternberg Astronomical Institute, Moscow State University, Universitetsky pr., 13, Moscow 119992, Russia
eshaldenkova@gmail.com
We consider the new method for atomic hydrogen de�ciency estimations. The main idea is to use the
empirical relation between total HI mass and speci�c angular momentum of the disk for isolated galaxies.
The method was compared with the standard one, based on dependence of HI mass on optical diameter and
galaxy type. They both were applied to Virgo and Coma cluster galaxies and to Local Volume galaxies. Also
we investigated possible mechanisms responsible for HI de�ciency in cluster spirals.
Introduction
In the dense regions of rich clusters galaxies interact with gravitational �eld of cluster, with each other
and with intergalactic medium. These interactions may a�ect physical properties and evolution of galaxies.
In di�erent works several mechanisms were investigated which may be responsible for HI de�ciency in cluster
galaxies (see, e.g., [1, 2, 8, 11, 20], [13]-[17]).
Cluster galaxies have, in average, a lower atomic gas content than their isolated counterparts. HI de�ciency
parameter was for the �rst time de�ned in [7] as logarithmical di�erence between observed HI mass and
expected one. The latter is estimated by empirical relation between HI mass and luminosity, type, and
optical linear diameter of the disk. This relation was obtained for isolated galaxies from Karachentseva
catalog [10]. Galaxies with |def HI| < 0.3 are considered as normal.
In our work we used semi-empirical relation between MHI and speci�c angular momentum of the disk
considered in [9],[22]-[24]:
(lgMHI)exp ≈ a + blgVRDC , (1)
where DC is optical linear diameter of the disk or scalelength, VR is rotational velocity of the disk on the
radius DC/2, a and b are some constants, and b ≈ 1.
Isolated and neighbouring galaxies
We obtained the dependence of HI mass on speci�c angular momentum of the disk for isolated galaxies
from AMIGA catalog [21] and for neighbouring isolated galaxies from Karachentsev et al. catalog [9] with
types from Sbc and later (Fig. 1).
We used galaxies with inclination angles not less than 30◦, and types from Sbc and later (t ≥ 3.5,
according to de Vaucouleurs [3]). We obtained the following empirical relation with correlation coe�cient
R = 0.94:
(lgMHI)exp = (1.06± 0.02)lgVRDC + (5.94± 0.06), (2)
where DC is diameter of galactic disk up to isophote 25 mag/arcsec2, in kpc, corrected for inclination and
extinction, VR is maximum deprojected rotation velocity (km/s) of the gas calculated from both the 21-
cm line widths at di�erent levels and/or the available rotation curves (generally Hα rotation curves) and
corrected for inclination, MHI is HI mass, obtained from corrected for self-absorption e�ect HI line magnitude,
in solar masses. All used quantities were taken from Hyperleda database [25].
This relation is also valid for Sab and Sbc galaxies. However galaxies with S0a-Sab (t = 0 − 2) types
show, on average, signi�cant lack of HI compared with later type galaxies. Hence we cannot apply considered
relation for most part of these galaxies.
The HI de�ciency parameter is de�ned as logarithmical di�erence between observed HI mass and expected:
(def HI)V D = (lgMHI)exp − (lgMHI)obs, (3)
23
Advances in Astronomy and Space Physics E. S. Shaldenkova
where (lgMHI)exp is logarithm of expected HI mass (in solar masses) of galaxy according to (2) and (lgMHI)obs
is logarithm of observed HI mass (in solar masses) of galaxy.
We estimated HI de�ciency for non-isolated galaxies from Karachentsev et al. catalog [9] and found no
correlation with the isolation degree. Therefore, processes responsible for HI de�ciency in cluster galaxies,
are not signi�cant in nearby groups.
HI de�ciency in cluster galaxies
For galaxies in Virgo and Coma clusters we estimated (def HI)V D using relation (2), obtained for isolated
galaxies. In Virgo we used galaxies from inner region of cluster, up to 1.8 Mpc; in Coma we used galaxies
up to 6 Mpc from cluster center, but within accepted cluster limits [12]: V = 5300 − 9000 km/s, α =
12h30m − 13h30m, δ = 26◦ − 31◦). MHI, VR and DC were taken from Hyperleda database [25]; we used
galaxies with inclination angles i > 30◦.
Diagrams �(def HI)V D�(def HI)Gavazzi� for Virgo and Coma cluster galaxies are presented in Fig. 2.
(def HI)V D is HI de�ciency obtained on the basis of HI mass dependence on speci�c angular momentum
of the disk, (def HI)Gavazzi is HI de�ciency from [5] (for Virgo) and [6] (for Coma).
Also we obtained a well-known relation between the mean HI de�ciency and clustercentric distance for
our method of HI de�ciency estimation (Fig. 3). In Virgo cluster we see a substantial HI de�ciency up to
nearly 2 Mpc from the cluster center, in Coma � up to 3 − 4 Mpc from the cluster center. Many galaxies
have normal hydrogen content at all distances.
The condition of disk gas stripping by ram pressure is given by the equation:
Pram ≥ 2πGΣstarΣgas.
Ram pressure Pram is given by:
Pram = ρIGMV 2
gal.
Typical ram pressure on distances where substantial HI de�ciency is observed (2 Mpc for Virgo and 3−4 Mpc
for Coma) for typical values Vgal = 1000 km/s, ρIGM = 10−4 cm−3 (see [4, 18]) is Pram ' 10−12 dyn/cm2.
But this value of ram pressure is not su�cient by order of magnitude for sweeping the considerable amount
of gas (see [19]). These galaxies either passed through the dense core of the cluster or HI de�ciency is related
with other reasons, for example with starvation e�ect.
Results and conclusions
1. Application of semi-empirical relation between total HI mass and speci�c angular momentum of the
disk for isolated Sab-Irr galaxies allowed us to estimate HI de�ciency in cluster galaxies without taking
into account their morphological types.
2. Neighboring galaxies from Karachentsev et al. (2004) catalog show no systemic HI de�ciency. Mean
deviation of HI mass from �normal� one is small and shows no correlation with isolation degree.
3. The relation between HI de�ciency and distance from cluster center was con�rmed for Virgo and Coma
cluster galaxies. We found out the existence of substantial HI de�ciency up to nearly 2 Mpc from
cluster center in Virgo, and up to 3− 4 Mpc from cluster center in Coma.
4. In Virgo cluster at distances where galaxies with substantial HI de�ciency are being observed the ram
pressure is not su�cient for sweeping o� considerable amount of gas. These galaxies either passed
through the dense core of the cluster or HI de�ciency is related to other reasons, for example with
starvation.
Acknowledgement
I would like to thank my research supervisor Prof. A. V. Zasov. I also appreciate to authors for the
possibility to use Hyperleda database.
24
Advances in Astronomy and Space Physics E. S. Shaldenkova
Figure 1: Diagrams �HI mass � speci�c angular momentum� for isolated galaxies with t ≥ 3.5 (left) and t = 0−3.5
(right).
Figure 2: Diagrams �(def HI)V D − (def HI)Gavazzi� for Virgo (left) and Coma (right) cluster galaxies. Straight
line corresponds to the equality of values.
Figure 3: Diagrams �def HI � distance from the cluster center� for Virgo (left) and Coma (right)
25
Advances in Astronomy and Space Physics E. S. Shaldenkova
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| id | nasplib_isofts_kiev_ua-123456789-118976 |
| institution | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| isbn | 987-966-439-367-3 |
| language | English |
| last_indexed | 2025-11-26T14:23:46Z |
| publishDate | 2011 |
| publisher | Advances in astronomy and space physics |
| record_format | dspace |
| spelling | Shaldenkova, E.S. 2017-06-02T18:30:05Z 2017-06-02T18:30:05Z 2011 Atomic hydrogen deficiency in spiral galaxies in clusters / E.S. Shaldenkova // Advances in Astronomy and Space Physics. — 2011. — Т. 1., вип. 1-2. — С. 23-26. — Бібліогр.: 25 назв. — англ. 987-966-439-367-3 https://nasplib.isofts.kiev.ua/handle/123456789/118976 We consider the new method for atomic hydrogen deficiency estimations. The main idea is to use the empirical relation between total HI mass and specific angular momentum of the disk for isolated galaxies. The method was compared with the standard one, based on dependence of HI mass on optical diameter and galaxy type. They both were applied to Virgo and Coma cluster galaxies and to Local Volume galaxies. Also we investigated possible mechanisms responsible for HI deficiency in cluster spirals. I would like to thank my research supervisor Prof. A. V. Zasov. I also appreciate to authors for the possibility to use Hyperleda database. en Advances in astronomy and space physics Advances in Astronomy and Space Physics Atomic hydrogen deficiency in spiral galaxies in clusters Article published earlier |
| spellingShingle | Atomic hydrogen deficiency in spiral galaxies in clusters Shaldenkova, E.S. |
| title | Atomic hydrogen deficiency in spiral galaxies in clusters |
| title_full | Atomic hydrogen deficiency in spiral galaxies in clusters |
| title_fullStr | Atomic hydrogen deficiency in spiral galaxies in clusters |
| title_full_unstemmed | Atomic hydrogen deficiency in spiral galaxies in clusters |
| title_short | Atomic hydrogen deficiency in spiral galaxies in clusters |
| title_sort | atomic hydrogen deficiency in spiral galaxies in clusters |
| url | https://nasplib.isofts.kiev.ua/handle/123456789/118976 |
| work_keys_str_mv | AT shaldenkovaes atomichydrogendeficiencyinspiralgalaxiesinclusters |