High Galactic Latitude Interstellar Neutral Hydrogen Structure and
  Associated (WMAP) High Frequency Continuum Emission
Revised, July 15, 2007
High Galactic Latitude Interstellar Neutral Hydrogen Structure
and Associated (WMAP) High Frequency Continuum Emission
Gerrit L. Verschuur
Physics Department, University of Memphis, Memphis, TN 38152 gverschr@memphis.edu
ABSTRACT
Spatial associations have been found between interstellar neutral hydrogen
(HI) emission morphology and small-scale structure observed by the Wilkinson
Microwave Anisotropy Probe (WMAP) in an area bounded by l = 60◦ & 180◦, b
= 30◦ & 70◦, which was the primary target for this study. This area is marked by
the presence of highly disturbed local HI and a preponderance of intermediate-
and high-velocity gas. The HI distribution toward the brightest peaks in the
WMAP Internal Linear Combination (ILC) map for this area is examined and by
comparing with a second area on the sky it is demonstrated that the associations
do not appear to be the result of chance coincidence. Close examination of several
of the associations reveals important new properties of diffuse interstellar neutral
hydrogen structure. In the case of high-velocity cloud MI, the HI andWMAP ILC
morphologies are similar and an excess of soft X-ray emission and Hα emission
have been reported for this feature. It is suggested that the small angular-scale,
high frequency continuum emission observed by WMAP may be produced at
the surfaces of HI features interacting one another, or at the interface between
moving HI structures and regions of enhanced plasma density in the surrounding
interstellar medium. It is possible that dust grains play a role in producing the
emission. However, the primary purpose of this report is to draw attention to
these apparent associations without offering an unambiguous explanation as to
the relevant emission mechanism(s).
Subject headings: Interstellar matter, neutral hydrogen, cosmology, WMAP
1. Introduction
Examination of the Wilkinson Microwave Anisotropy Probe (WMAP) images immedi-
ately fires the imagination, especially the summary image that has received so much publicity,
http://arxiv.org/abs/0704.1125v2
– 2 –
the so-called Internal Linear Combination (ILC) map (Hinshaw et al, 2006). It is readily
accessed at http://map.gsfc.nasa.gov and was produced after subtraction of suspected galac-
tic components from the 5-channel observations carried out by WMAP and then combining
the data. But do the remaining structures in the ILC map truly reveal the fingerprints of
processes that took place shortly after the universe was born? Upon close inspection, certain
features in the WMAP ILC map (hereafter the ILC map) look hauntingly familiar to those
who have spent their careers studying Galactic, interstellar neutral hydrogen (HI) structure.
This can be recognized in a visual comparison of the above-referenced ILC image and the
all-sky HI column density map found at http://www.astro.uni-bonn.de. Several extended
areas of excess emisison at high galactic latitudes (b >30◦) are present in both maps; for
example in the areas around galactic longitude and latitude (l,b) = (170◦,80◦), which exhibits
extensive intermediate- and high-velocity HI, and around (l,b) = (160◦,-35◦). Also, a striking
area of extended ILC structure that reaches from (l,b) = (230◦,0◦) through (l,b) = (315◦,-
35◦) has a counterpart in the HI data where a tongue of emission follows roughly the same
axis, emerging from the galactic disk HI at (l,b) = (255◦,-15◦) and stretching through (l,b) =
(310◦,-35◦). These apparent associations initiated a closer look at the HI structure and ILC
data for several areas of sky. If the ILC small-scale structures correspond to cosmological
signals, absolutely no associations with HI structure, other than those due to pure chance,
should be found.
The thrust of this paper is to highlight the fact that a close relationship between ILC and
HI structures appears evident in the data. This deserves closer attention. Lagache (2003)
has examined the relationship between WMAP structure and interstellar HI by considering
the HI emission integrated over all velocities as a function of position and suggests that
excess WMAP emission may be associated with small, transiently heated, dust particles. In
the data presented below, the apparent associations are found by examining HI area maps
produced by integrating over limited velocity ranges as opposed to the total HI content.
Small-scale HI features due to relatively weak and narrow emission profile structure tend to
become lost when maps of integrated HI content are plotted.
In §2 the data and analysis are described. In §3 several of the most informative exam-
ples of close correspondences and morphological associations between HI and ILC structure
are presented. In the discussion in §4 reference is made to possible, dust-related emission
mechanisms that may be invoked to account for the associations and a geometric model for
producing the apparent morphological associations is outlined. In the conclusions in §5 the
hope is expressed that others will be motivated to seek confirmation (or otherwise) of the
claims made here.
http://map.gsfc.nasa.gov
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2. Data and Analysis
The goal of the present study was to determine if parallels exist between small-angular-
scale (1◦ to 2◦) galactic HI structure and high-radio-frequency continuum emission features
observed by WMAP. Neutral hydrogen emission profile data with an angular resolution of
0.6◦ were obtained from the Leiden-Dwingeloo, sidelobe-corrected HI Survey (Hartmann &
Burton, 1997) as well as the more extensive Leiden-Argentina-Bonn (LAB) All-Sky Survey
(Kalberla et al. 2005). In our study the distribution of the HI brightness was initially
plotted as a function of galactic longitude and latitude (l,b maps) every 10 km/s in velocity
integrating over a 10 km/s range. The focus of the first phase of this study is Region A,
bounded by l = 60◦ & 180◦, b = 40◦ & 70◦ for which 25 maps covering the velocity range of
-200 to +50 km/s with respect to the local-standard-of-rest were produced.
The HI and ILC data in the form of l,b maps were visually examined in a manner
akin to blink comparison using a transparent overlay of the ILC data to search for apparent
associations between small–scale structures. The galactic HI sky is filled with small-scale
structure evident in such l,b maps (e.g., see Hartmann & Burton, 1997) so that any attempt
to compare with small-scale structure found in the ILC data, which also consists of many
small peaks of order 1 to 2◦ across, will lead to chance agreements in position. This was
tested (to first-order) by also comparing the ILC map for the Region A data with the HI l,b
maps for Region B, chosen as l = 180◦ to 300◦, b = 40◦ to 70◦. This is located symmetrically
opposite the galactic anti-center with respect to the Region A. To this end, 20 HI maps from
-120 to +80 km/s at 10 km/s intervals were produced to cover the extent of the galactic HI
emission in Region B.
For Regions A & B, lists of the brightest ILC peaks were produced. For Region A
this included all 51 ILC peaks with amplitudes ≧0.100 mK. For Region B, 51 peaks were
also used whose amplitudes are ≧0.117 mK. The centers and amplitudes of the ILC and
the apparently associated HI peaks were recorded and the angular separations between the
ILC and apparently associated HI peaks calculated. The same was done for two lists of 51
negative amplitude ILC peaks for Regions A & B whose amplitude limits are ≦-0.131 &
≦-0.144 mK respectively.
2.1. Statistics of the Apparent Associations
The morphologies of both HI and ILC structures are complex yet distinct brightness
features of a small angular extent of order 1◦ to 2◦ are common in both classes of data. To
derive a rough estimate of the likelihood of finding chance associations between ILC and
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HI peaks it is possible to calculate how likely it is that one of NWpeaks in the ILC map will
coincide by chance with one of NHpeaks in the HI maps for the the same area, A, assuming
both to be randomly distributed on the sky.
The number, N, of HI peaks expected to lie by chance within a distance r of any ILC
peak, that is within an area of order π r2 square degrees centered on the ILC peak, is given
N = πr2A−1NWpeaks NHpeaks. (1)
This is a first-order approach to the problem and ignores an edge-effect that will be
introduced for large separations, r, which reduces the effective area, A, to be entered in
Eqtn. 1. At small separations this is a minor correction. This estimate is in any case limited
for several other reasons. For example, the two classes of structure are treated as being
random on the sky, which is not so for HI, because it is known to be filamentary. Also, the
apparent associations that are found (see Table 1 below) are spread over all velocities with
associations at anomalous velocities relatively over-represented in Region A. In addition, no
account is taken of morphological similarities between the two types of structure other than
to search for sets of closed contours on a scale of 1◦ to 2◦. Morphological similarities reported
in §3.3 below are difficult to quantify in a formal manner but in any event would reduce the
likelihood of chance associations.
For each of the HI maps about 10 to 15 contour levels were plotted and the number of
peaks, defined as sets of closed contours with dimensions of order 1◦ to 2◦, was counted on
each of the HI maps. A given HI peak on one contour map can usually be followed over at
least two or three adjacent maps for HI at velocities outside ± 20 km/s with respect to the
local-standard-of-rest. In one case the relevant HI peak could be followed over as many as 8
maps (i.e., 80 km/s). Furthermore, low velocity HI (−20 < v < 20 km/s), narrow emission
line components of order 6 km/s wide tend to appear in only one contour map integrating
over a 10 km/s width. On average, each HI peak is identified in 2 adjacent velocity maps so
that the value of NHpeaks is this half of the number found in all the HI l,b maps used in the
analysis.
In the case of Region A, about 452 obvious HI peaks in the 25 area maps were counted,
which sets NHpeaks = 226. For Region B the HI is more highly concentrated to low latitudes
and low velocities and fewer HI peaks were counted in the 10 km/s wide HI maps at b≧40◦.
Using the same criterion that on average an HI peak can be followed over 2 adjacent HI
maps, NHpeaks = 130 is used in the calculations.
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2.2. The Angular Distribution of Apparent Associations
In Fig. 1 the distribution of the angular offsets in 0.◦2 bins between ILC and HI features
for a number of data comparisons are shown. Fig. 1(a) presents the histogram of angular
separations between ILC and HI peaks when the ILC peaks for Region A are compared to
the HI data for Region A. It shows a clear excess at small angular separations with the peak
occurring at about 0.◦8, only slightly larger than the beamwidth. Beyond 1◦ separation,
the values fall below expectations for chance associations indicated by a dashed line that
represents Eqtn. 1. Of the 51 ILC peaks in Region A, some 60 associations make up the
histogram. As will be discussed below, this carries a clue to the nature of the phenomenon
producing the associations.
A similar excess of offsets between ILC and HI peaks with small angular separations
is seen in Fig. 1(b) for Region B, which shows the results obtained by overlaying the ILC
data on the HI maps for the same area. The numbers involved are smaller than for Region
A with the bulk of the HI concentrated to low velocities.
An estimate of the significance of the apparent associations found in Figs. 1(a) and (b)
can be obtained by overlaying the ILC data for Region B on the HI peaks for Region A,
and vice versa. Figure 1(c) shows what is found when the Region B ILC peaks are overlain
on Region A HI maps. Figure 1(d) shows the converse. Neither plot shows evidence for
systematic small-scale angular offsets other than might be expected from chance.
Finally, negative ILC peaks and HI structure were compared. Figure 1(e) shows the
results found by overlaying Region A negative amplitude peaks on Region A HI maps and
Fig. 1(d) shows the results derived by overlaying Region B negative ILC peaks on HI data
for the Region B. Fig. 1(g) plots the results obtained when comparing the negative ILC
peaks for Region B with the HI for Region A and Fig. 1 (h) shows the converse. None
of these four plot show convincing evidence for systematic small-scale angular offsets other
than might be expected from chance.
Another way to summarize these results is to compare the total number of cases of
close associations at small angular separations. For example, for those offset by 1.◦1 or less,
Region A contains 41 cases, compared to the 23 estimated from chance according to Eqtn.
(1), which compares to 20, 17, 21 cases for the plots in Figs. 1 (c),( e) & (g), which are
independent estimates of what is to be expected due to chance associations. Similarly, for
Region B the direct comparison produces 22 cases of small offsets compared to 13 predicted
by chance, with the other three comparisons summarized in Figs. 1 (d), (f) &(h) producing
10, 9 & 6 cases respectively. This suggests that the close associations found in Region B are
also significant.
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These plots point to the possibility that the ILC continuum peaks are located at the
boundaries of galactic HI emission features, which implies at the interface between HI struc-
tures and surrounding plasma, or at the interface between colliding HI structures.
3. Case Studies of Associated HI and Continuum Structures
If the close associations between ILC and HI structures found especially in Region A are
indeed significant then they should be expected to reveal underlying aspects of interstellar
gas dynamics that may allow the cause of the relationships to be understood. That would
then remove the study from the realm of a statistics to that of interstellar physics.
The cases outlined below emerged from the study of an extended version of Region
A with the latitude boundary set to 30◦. Table 1 lists the apparent associations with an
identifying number for the ILC peak given in column 1 and its galactic coordinates (in
degrees) in columns 2 & 3. The peak ILC brightness temperature in mK is given in column
4. Column 5 gives the center velocity in km/s with respect to the local standard of rest
of the HI map used to determine the positions of the relevant HI feature; hence -95 km/s
refers to the HI map integrating from -100 to -90 km/s. Columns 6 and 7 give the galactic
coordinates for the HI peak with the amplitude in units of K.km/s in Column 8. The angular
offset in degrees between associated peaks is given in Column 9.
Table 1 includes 64 ILC peaks with amplitudes ≧0.100 mK. All but two of these appear
to have associated HI peaks yet the table includes 83 entries for HI associated with the
remaining 62 ILC peaks. This is consistent with multiple HI structures being involved in
creating some of the continuum emission peaks.
In those directions where the most dramatic associations between ILC and HI structure
were noted, the HI data were examined in more detail by using HI maps made by integrating
over 5, 2 or 1 km/s and latitude-velocity b,v plots with a view to obtaining further insights
into the nature of the possible relationship between the two forms of emission.
In most of the plots below, the ILC data are shown as contours overlain on the HI
morphology plotted using inverted gray-scale shading and these examples are offered be-
cause they each reveal something interesting and unexpected about the nature of interstellar
matter. This is regarded as highly significant because these directions would never have
been chosen for closer study if it were not for the apparent associations with the continuum
emission peaks highlighted in the ILC map.
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3.1. Source 25 at (l,b) = (112.◦3,57◦.8): Directly overlapping HI and
continuum features
Figure 2(a) shows the brightness of a high-velocity (v ≦-100 km/s) HI feature # 25 from
Table 1 centered at -118 km/s integrated over 5 km/s (peak value 51 K.km/s). Fig. 2(b)
shows the brightness of an intermediate-velocity (between -100 and -30 km/s) HI feature
centered at -87 km/s integrated over 5 km/s (peak value 47 K.km/s). By using Gaussian
analysis of the HI profiles every 0.◦5 in latitude and longitude across the peaks, the coordi-
nates of the centers of the HI structures were accurately derived and found to be identical
in latitude (to < 0.◦1) and also identical to the latitude center of the ILC peak. The centers
of two HI features are identical in longitude but offset from the ILC peak by 0.◦3, half the
the beamwidth used in the HI studies.
Examination of the latitude-velocity b,v plot at l = 112◦ for this feature revealed no
significant HI emission at -100 km/s between the two peaks seen in Figs. 2(a) and (b).
However, a marked lack of low-velocity HI emission around zero velocity is revealed. (Low-
velocity is defined as between + 30 and -30 km/s.) Fig. 2(c) shows the integrated HI content
over the velocity interval -8 to +2 km/s with the continuum contours overlain. The peak in
the ILC structure is clearly co-located with a lack of low-velocity HI. Also at low velocities an
HI peak at (l,b) = (115◦, 57◦) is associated with a secondary peak in the continuum emission.
Further relationships emerge when the integrated HI emission between -130 & -120 km/s is
examined, Fig. 2(d). Two HI maximum at (l,b) = (113◦,55◦) and (l,b) = (115◦,54◦) overlie
HI minima seen in Fig. 2(c).
These plots suggest a direct relationship between high- and intermediate-velocity HI
and a distinct minimum in low-velocity HI, with all of them related to the presence of an
ILC continuum emission peak. This contrasts with those models that would place the high-
and intermediate-velocity HI at very different distances well removed from local HI. For
example, Wakker (2001) places the high-velocity gas at distances of several kiloparsecs with
the intermediate-velocity HI at about 1 kpc, both of which contrast with the realm of high-
latitude, low-velocity H, which is local at distances of order 50 to 100 pc. Blaauw & Tolbert
(1966) originally noted that intermediate-velocity HI and a relative lack of low-velocity gas
is a hallmark of that area of sky encompassed by Region A, which places them both within
about 100 pc of the Sun. Here we find striking evidence in Fig. 2 that HI structure in
all three velocity regimes is related, something that would not have been noticed but for
the apparent association with a significant peak in the ILC structure. This implies that HI
gas in all three velocity regimes in this direction is local. (The possibility that small-scale,
intermediate-velocity structure is associated with a lack of low-velocity gas has been briefly
noted by Burton et al. (1992) as well as Kuntz & Danly (1996) without their following up
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on the implications.)
3.2. Sources 11 & 31 centered at (l,b) = (119.◦5, 57◦) and association between
high- and low-velocity HI
Figure 3(a) shows the HI structure of high-velocity gas integrated between -140 and
-110 km/s associated with two ILC continuum peaks, 11 & 31 (Table 1) identified in Fig.
3(b). The ILC peaks are linked by a ridge of emission straddled by two HI features (peak
amplitudes 22 K.km/s) whose morphologies closely follow the continuum radiation contour
lines. Gaussian analysis of the HI profiles in a 0.◦5 grid for the entire area covered in Fig. 3(a)
was carried out and allowed the center velocities of the two HI components to be determined.
They are -127 and -118 km/s for the northern and southern peaks, respectively. The Gaussian
analysis also allowed the HI column density for two other features to be mapped, shown in
Figs. 3 (b) and (c). Their presence was recognized in a set of HI emission profiles at l=120◦
shown in Fig. 3(d). Most striking is a component at -8 km/s, that is seen only at (l,b) =
(120◦,57◦). It has a peak column density of 7×1018 cm−2 and its morphology is plotted in
Fig 3(b), which shows that it is located precisely on the saddle in the continuum contours
between two peaks. Even more striking is the fact that it is unresolved in angle.
Fig. 3(c) shows the column density plot for the -17 km/s feature evident in Fig. 3(d),
again based on the results of the Gaussian analysis of the area profiles (peak column density
19×1018 cm−2). The location of this component also appears related to the presence of the
continuum ridge with the southern peak located at the position of the HV peak that nestles
in the indentation (or pinch) in the continuum emission ridge. At this stage of the analysis,
no clear relationship between intermediate-velocity HI structure and other features in the
area of Fig. 3 has been noted. However, very weak positive velocity HI emission is also
found toward this structure but it will require confirming observations to determine if it is
real.
The plots in Fig. 3 represent the second example of a close relationship between HI
structures at low- and high-velocities, with each of them related to the presence of an ILC
feature. In addition, the discovery of the angularly unresolved, low-velocity, high-galactic-
latitude emission peak is unprecedented and deserving of observations at much higher angular
resolution.
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3.3. Continuum source 33 at (l,b) = (89.3◦, 34.5◦) and associated
high-velocity HI
Figure 4 illustrates the dramatic association between ILC emission peak 33 (Table 1)
and HI. Here nine inverted gray-scale images of the HI at different velocities are overlain by
a contour map of the ILC structure. All the HI plots are single channel maps (1 km/s wide)
and the peak brightness temperatures are of order 0.8 K, except for the map at -200 km/s
where the peak is 0.3 K and at -150 km/s where it is 1.1 K. The limits of the associated HI
emission are -135 km/s at the same location as the peak at -140 km/s, and -205 km/s. The
HI centroid of emission shifts in velocity as it follows the ridge of the ILC emission feature
with a bifurcation of the HI peak starting at -170 km/s to produce two components that
”move” along opposite sides of the continuum ridge as the velocity is increased.
A preliminary attempt to sketch the structure revealed in these and HI l,b maps at
smaller velocity intervals suggests a twisted pattern around an axis defined by the contin-
uum radiation, possibly related to helical magnetic field structure around this axis. Higher
resolution HI data are desirable to untangle the HI structure in this fascinating area. Note
that the map of total HI in these directions carries no hint of the existence of the structure
seen in Fig. 4 because it is very faint compared to low-velocity gas in this area of sky.
Examination of b,v plots and emission profile data for this area reveal further details that
are relevant to understanding the apparent relationship between HI and ILC features. This
is illustrated in Fig. 5(a) in which several HI emission profiles cutting across the continuum
feature seen in Fig. 4 are shown. In a manner similar to that reported in §3.2 above, a
distinct additional component, in this case at -40 km/s, emerges in one of the profiles. Its
morphology integrated between -42 to -38 km/s is shown in Fig. 5(b) as an inverted gray
scale image (peak value 6.7 K.km/s) with the same ILC contours shown in Fig. 4 overlain.
Fig. 5(c) illustrates in contour map form how closely this intermediate-velocity HI structure
(contours from 3 K.km/s in steps of 0.05 K.km/s) mimics the continuum contours seen in
(b). Their axes are aligned to better than 5◦. This HI component is clearly associated with
the continuum as well as the HI structure at high velocities seen in Fig. 4.
Further examination of the b,v contour maps reveals a phenomenon also found for the HI-
continuum association noted in §4.1 (Fig. 2) above, a dearth of low-velocity emission where
the anomalous velocity HI structure shows a peak. This is illustrated in Fig 5(d) where the
integrated HI emission from -5 to +15 km/s (peak 36 K.km/s) is shown. A distinct minimum
(36 K/km/s) compared to the maximum value in this plot (112 K.km/s) in the low velocity
integrated HI emission is found at the location of the peak in the intermediate-veloicity HI
emission at -40 km/s. This, in turn, coincides with the location of continuum source 32 and
the HV structure seen in Fig. 4.
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3.4. Close-up view of HVC MI
Figure 6 shows the inverted gray-scale image of the HI brightness associated with high-
velocity cloud MI integrated over the velocity range -140 to -100 km/s. The double HI peaks
are offset from and parallel to a pair of ILC peaks, sources 19 and 57. A third ILC peak 43
is also associated with a weak HI feature, see Table 1. This main double HI feature is well
known and corresponds to high-velocity cloud HVC MI.
A crucial clue as to the likely cause for associations between the small-scale HI and high-
frequency continuum structures is found in a report of excess soft X-ray emission toward HVC
MI found by Herbstmeier et al. (1995). Their Figure 7a has been adapted to correspond to
the data in Figs. 6(a) & (b) and is shown as Fig. 6(c) where the contours correspond to the
HI emission from HVC MI similar to the data in (a). The shaded pixels overlain correspond
to areas of excess soft X-ray emission. Furthermore, Tufte, Reynolds & Haffner (1998)
have reported excess Hα emission at several positions toward HVC MI. The close spatial
relationship seen in Fig. 6(c) between the X-ray hot spots and the HI and the high-frequency
continuum emission observed by WMAP, as well as the presence of Hα emission contains
critical clues that should lead to understanding the nature of the associations between HI
and weak, high-frequency continuum emission. It is predicted that high-velocity cloud MII,
a companion to MI but located outside Region A, will show a similar relationship between
HI and ILC structures. (The outcome of this prediction will be discussed in a future report.)
In Fig. 6(d) the ILC contours are overlain on the low-velocity HI data. Again a relative
lack of LV emission, here integrated between 5 & +5 km/s, is seen to be closely associated
with the continuum and HI structure at high velocities. The HI column density is 1.8 K.km/s
for the minimum compared to 6.2 K.km/s for the maximum at the top left of (d).
4. Discussion
Several authors have considered the possibility that excess WMAP emission may be
produced by spinning dust grains, in turn possibly associated with HI. For example, Davies
et al. (2006) note that the spectrum of the low WMAP frequency data is consistent with
such a model. In contrast, Banday et al. (2003) find evidence in earlier COBE data of a
component in the continuum emission with a dust-like morphology but with a synchrotron-
like spectrum. Larson & Wandelt (2004) have suggested that both the ILC data positive
and negative peaks do not have sufficient amplitude to be accounted for by a cosmological
interpretation of the data, which implies some other mechanism may be playing a role in
generating the observed signals. In a specific case involving the detection of anomalous
– 11 –
microwave emission toward the Perseus molecular cloud, Watson et al. (2005) present an
hypothesis that dipole emission from spinning dust grains can account for the spectrum of
the continuum emission in the range 10 to 50 GHz. An extensive literature exists concerning
the possible role of spinning dust grains as the cause of continuum emission in the frequency
range of the WMAP experiment. This includes Draine & Lazarian (1998), Finkbeiner at al.
(2002), Schlegel et al. (1998), and de Oliviera et al. (2005). An alternative mechanism for
producing low density electrons possibly capable of generating high-frequency radio emission
involves a plasma physical phenomenon suggested by Verschuur (2007).
In general, many high latitude ILC peaks listed in Table 1 for extended Region A have
a corresponding, closely-spaced HI peak found in two or more l,b maps made at 10 km/s
intervals. The typical angular offset is approximately 0.◦8 (Fig. 1a). Including the cases
below b = 40◦ in the statistics makes no difference to the distribution seen in Fig. 1a.
Angular offsets of order 1◦ between parallel HI, dust and Hα filaments have been reported
by Verschuur et al. (1992).
Based on the above results it is suggested that the ILC peaks are associated with HI
structures that are interacting (probably colliding) with other HI structures, or interacting
with regions of enhanced plasma density in surrounding interstellar space through which
the HI is moving. In one case illustrated above, two HI features at distinctly different
velocities are coincident in position at the location of the ILC peak, Fig.2. In other cases,
two HI features at (nearly) the same velocity straddle a continuum emission peak in position,
for example as shown in Fig. 3. Depending on the geometry of the situation, positional
coincidence will only be observed in those directions where a collision between two HI features
(clouds) occurs along the line-of-sight. However, where the HI features are interacting while
moving along an axis oriented at some angle to the line-of-sight, the continuum emission
peak will be observed as offset from the HI peak(s).
A number of clues that may help account for the physics underlying the production
of continuum emission at the surface of moving HI structures exist in the literature. For
example, as was described in §3.4, Herbstmeier et al. (1995) report excess soft X-ray emission
at the boundary of HVC MI where the ILC continuum structure is prominent (Fig. 6). On
a larger scale, Kerp et al. (1999) find evidence for widespread soft X-ray emission over much
of Region A toward the high-velocity structures but the angular resolution of their data do
not allow for closer comparison with our results. Furthermore, Tufte et al. (1998) found
Hα emission high-velocity clouds MI & MII as well as other high-velocity features. This
raises tantalizing questions as to the emission mechanism that could produce the continuum
radiation. If it involves the formation of dust at the (shocked) interface between the HI and
surroundings by a mechanism involving spinning dust grains such as has been proposed by
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Draine & Lazarian (1998), the presence of both excess Hα and soft X-ray emission will also
have to be taken into account.
Lagache (2003) has searched for associations between HI and WMAP peaks but confined
his study to the total HI content as a function of position. In the examples above the
amplitudes of the HI peaks show a relationship to ILC peaks that varies widely and in many
cases, such as for the HI features shown in Figs. 4 or 5, are invisible in maps of total HI
content over the relevant areas. Land & Slosar (2007) also studied the relationship between
WMAP peaks and HI structure but considered only direct, point-to-point associations that
are in fact relatively rare. Far more likely are small angular offsets between peaks in the two
forms of emission.
Another interesting, possibly related phenomenon, has been found by Liu & Zhang
(2006) who studied the cross-correlation betweenWMAP and Egret γ ray data and concluded
that an unknown source of radiation, most likely of galactic origin, is implied by their
analysis. Such a source would produce foreground residuals that need to be removed in
order to minimize their role in confusing the cosmological interpretation of the WMAP data.
Perhaps the source of this unknown radiation of galactic origin is to be found in processes
occurring at the surfaces of Galactic HI structures moving through interstellar space and/or
interacting with one another.
Based on what is found in these examples, it is possible that where two HI features are
interacting (colliding) current sheets are created in which particle acceleration may underlie
the production of the continuum emission observed by WMAP. Excess electrons at these
interfaces may initially be introduced through the process described by Verschuur (2007)
and references therein.
To pursue this study this further, ILC structure should be compared with l,b HI maps
integrated over smaller velocity ranges that the 10 km/s used in this overview and higher
angular resolution HI observations of some of the most interesting HI features shown in Figs.
2 to 6 are desirable. It is hoped that research into the relationships between interstellar HI
morphology and high-frequency radio emission observed by WMAP will be stimulated by
this work.
5. Conclusions
The goal of this study was to determine if evidence exists to suggest that small-scale
structure in the WMAP ILC data and HI are related. To that end, the map of ILC structure
guided the study and led not only to the discovery of what appear to be highly significant
– 13 –
spatial relationships between the two data sets but also drew attention to unexpected proper-
ties of the galactic HI that turned out to be especially interesting and relevant to accounting
for the associations.
In Region A clear associations have been found between small-scale structure observed
by WMAP and galactic HI features identified in maps in which the HI is integrated over
10 km/s. In Region B a similar excess of associated features was noted. In contrast, no
significant associations are found when comparing the ILC data for one Region with the
HI data for the other Region, nor when the minima in the ILC data are treated as peaks.
This argues that the apparent associations found in Region A are not due to chance. While
studying the data for Region B in which the HI is more concentrated to low velocities and
latitudes it became clear that HI maps at smaller velocity intervals should be used in the
search for associations. A future report will describe such work together with extensive
studies of structures at high latitudes in the southern galactic hemisphere.
Taken as an ensemble, the spatial associations between HI and ILC emission peaks point
to the existence of one or more processes occurring in interstellar space capable of generating
weak continuum radiation observed by WMAP. The radiation appears to originate at the
surfaces of dynamic and interacting HI structures. Where this interaction is viewed along
the direction in which the HI is moving the radio continuum structure will overlap in position
but where the HI has a transverse component of motion (much more common) the two forms
of emission will appear closely offset on the sky.
Of particular significance is the fact that the associations between ILC and HI structure
discussed here led to the discovery that HI structures in the three velocity regimes (high,
intermediate and low) are physically related to one another, which places them at a common
distance from the Sun, probably of order 100 pc.
Rigorous studies of the apparent associations between ILC and HI structures should
make use of the full LAB survey spectral resolution of 1 km/s to produce HI maps integrating
over 2 km/s velocity intervals, a limit set by what is known about low-velocity HI emission
line structure.
I am grateful to Wayne Landsman and Gary Hinshaw for the first-year ILC continuum
emission data in digital form and in rectangular coordinates. The encouragement and advice
offered by an anonymous referee as well as Richard Lieu as this paper evolved to completion
was essential to its progress. I am particularly grateful to Tom Dame for providing me with
the necessary software for a Mac computer to allow the production of the vast majority of
the final area maps of HI emission presented in this paper. I also greatly appreciate en-
couragement from and discussions with Joan Schmelz and Butler Burton and the important
– 14 –
feedback offered by Dave Hogg, Mort Roberts, Ed Fomalont, Eric Priest, Petrus Martens,
Tony Peratt, Max Bonamente, Shuang-Nan Zhang & Eric Feigelson as well as numerous
audience members who attended seminars I gave in the early phases of this project.
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– 16 –
Table 1. TARGET AREA ASSOCIATIONS
No. l b ILC Temp. HI Velocity l b HI amplitude Angular offset
(1) (2) (3) (4) (5) (6) (7) (8) (9)
1 139.6 40.1 0.227 -55 139.2 40.5 37 0.50
1 139.6 40.1 0.227 5 139.6 41.0 139 0.90
2 174.4 56.8 0.223 -95 175.0 55.6 8 1.24
3 160.3 62.9 0.218 -115 163.0 64.0 6 1.65
3 160.3 62.9 0.218 -15 160.0 61.5 34 1.41
4 176.1 53.0 0.212 5 176.5 53.5 16 0.55
5 140.3 41.5 0.202 -45 140.3 41.0 24 0.50
6 172.3 59.5 0.199 -65 168.2 58.5 27 2.31
7 174.0 50.5 0.182 -125 171.5 51.4 4 1.83
7 174.0 50.5 0.182 -15 173.1 50.1 29 0.70
8 177.2 57.6 0.182 -105 175.5 55.5 8 2.29
9 168.1 67.4 0.180 -125 167.0 65.1 30 2.34
9 168.1 67.4 0.180 -25 168.2 66.5 26 0.90
9 168.1 67.4 0.180 -45 168.3 68.5 44 1.10
10 171.6 56.3 0.179 -65 170.8 56.0 16 0.54
10 171.6 56.3 0.179 -55 172.0 56.0 13 0.37
11 118.1 57.0 0.175 (-121) 120.0 58.0 1.1 1.44
11 118.1 57.0 0.175 (-115) 120.0 56.5 1.0 1.15
11 118.1 57.0 0.175 (-8) 120.0 57.1 1.8 1.04
12 159.6 50.0 0.172 none none none · · · · · ·
13 169.5 46.5 0.172 -15 167.5 47.6 42 1.76
13 169.5 46.5 0.172 -5 170.0 47.2 47 0.78
14 174.7 48.2 0.172 -15 175.5 46.5 28 1.78
15 174.4 31.8 0.172 -5 174.0 31.0 110 0.87
16 101.8 59.5 0.169 -5 100.8 58.5 32 1.12
17 78.2 55.9 0.168 5 78.5 56.0 62 0.20
17 78.2 55.9 0.168 -25 79.5 56.5 26 0.94
18 82.3 55.7 0.168 -15 80.0 56.7 35 1.64
19 165.7 64.8 0.168 -125 167.0 65.0 30 0.59
19 165.7 64.8 0.168 -15 165.9 65.4 18 0.61
– 17 –
Table 1—Continued
No. l b ILC Temp. HI Velocity l b HI amplitude Angular offset
20 91.5 36.7 0.166 -135 91.0 38.1 15 1.46
20 91.5 36.7 0.166 -35 91.1 37.9 17 1.24
20 91.5 36.7 0.166 -15 91.9 37.0 36 0.44
21 170.2 54.5 0.165 -55 170.0 55.0 9 0.51
21 170.2 54.5 0.165 5 169.6 55.9 17 1.44
22 135.4 51.1 0.164 -45 135.9 51.1 98 0.31
23 151.2 48.8 0.162 -165 152.3 48.5 4 0.78
23 151.2 48.8 0.162 -15 152.1 49.1 11 0.66
24 172.6 46.1 0.161 -15 173.3 46.0 22 0.50
25 112.3 57.8 0.159 (-87) 112.8 57.6 4.8 0.33
25 112.3 57.8 0.159 (-125) 112.1 57.9 9 0.15
26 62.6 42.9 0.157 -15 63.5 42.7 19 0.69
27 165.6 48.2 0.155 -15 166.2 48.0 26 0.45
28 65.0 37.1 0.155 -115 64.5 37.5 5 0.56
29 68.6 37.1 0.150 -145 66.6 37.0 5 1.60
30 93.2 66.6 0.150 -5 94.0 65.0 32 1.63
31 121.6 56.8 0.150 -140 to -110 see text see text see text 1.00
32 113.4 66.4 0.149 -15 115.4 66.0 22 0.90
33 89.3 34.5 0.146 (-170) 89.0 34.5 0.8 0.25
33 89.3 34.5 0.146 -42 to -38 89.4 34.5 7 0.08
34 158.8 32.0 0.145 -55 157.5 32.0 30 1.10
35 94.6 38.6 0.143 -165 94.7 38.0 4 0.61
36 77.0 46.9 0.143 -25 79.0 47.0 16 1.37
37 117.0 48.0 0.138 -85 117.5 47.3 19 0.78
38 78.2 62.5 0.138 -25 77.0 62.0 22 0.75
39 62.6 38.7 0.137 -15 61.1 39.5 22 1.42
40 167.3 55.7 0.136 -135 167.0 55.5 16 0.26
41 172.8 35.9 0.132 -5 172.0 36.0 25 0.66
42 174.7 63.6 0.131 -55 172.7 65.0 32 1.66
43 163.8 63.8 0.130 –125 162.1 63.6 4.5 0.78
44 131.8 57.6 0.128 -75 131.0 57.5 30 0.44
– 18 –
Table 1—Continued
No. l b ILC Temp. HI Velocity l b HI amplitude Angular offset
44 131.8 57.6 0.128 -115 133.0 57.0 33 0.44
45 125.2 40.0 0.127 -65 123.9 40.5 23 1.11
46 138.7 52.7 0.126 -55 139.3 52.5 16 0.41
47 166.3 34.6 0.125 -45 165.8 35.0 36 0.57
48 118.5 68.3 0.124 -25 119.0 68.0 19 0.35
49 132.9 50.0 0.122 none none none · · · · · ·
50 153.6 68.5 0.122 -85 155.1 67.5 20 1.14
51 159.3 56.1 0.120 -35 159.9 56.0 16 0.35
52 95.4 46.9 0.120 -115 95.0 46.0 7 0.94
52 95.4 46.9 0.120 -65 96.0 47.5 7 0.73
53 149.4 67.2 0.118 -5 149.6 67.5 56 0.31
54 160.7 57.4 0.115 -85 160.0 58.0 5 0.71
55 142.7 35.2 0.115 -25 143.7 34.5 12 1.20
56 167.3 61.6 0.114 -5 167.9 59.8 18 1.82
57 163.3 66.2 0.114 -125 165.0 66.4 25 0.71
58 140.7 67.0 0.109 -95 138.6 67.0 22 0.82
59 145.7 37.1 0.109 15 145.1 37.9 20 0.93
60 143.4 66.6 0.106 -95 146.3 67.3 14 1.35
61 146.3 36.5 0.105 -55 146.3 36.5 30 0.00
62 158.6 67.2 0.104 -95 160.6 66.0 14 1.43
63 164.2 69.1 0.103 -45 164.0 69.0 28 0.12
64 148.2 67.9 0.100 -85 146.5 67.5 23 0.75
– 19 –
Fig. 1.— The distribution of angular separations between ILC peaks and closely spaced HI
peaks for b ≧40◦for various combinations of ILC and HI data for the two Regions A &B,
see text. The dashed line represents a model calculation for a random distribution of peaks
according to Eqtn. 1, and the systematic excess of associations with low angular separations
with respect to the model in the top two plots supports the hypothesis that the continuum
emission arises at the surfaces of HI features.
– 20 –
Fig. 2.— ILC peak 25 from Table 1 at (l,b) = (112.◦3, 57.◦8) at the center of the map
(contours from +0.04 in steps of 0.02 mK) overlain on HI (inverted gray scale) structure at
the velocities indicated. In (a) the ILC peak is associated with a high-velocity HI feature
and in (b) with an intermediate-velocity HI feature. In (c) the ILC peak is compared to low
velocity HI and overlies a clear HI deficit. It is striking that the integrated high-velocity HI
emission displayed in (d) shows two other peaks that are co-located with minima in (c), see
text. These structures strongly suggest that the anomalous velocity gas is interacting with
low-velocity HI, producing the ILC continuum emission in the process.
– 21 –
Fig. 3.— (a) The ILC peaks 11 & 31 from Table 1 labeled in (b) with contour levels from
0.02 mK in steps of 0.03 mK centered at (l,b) = (120◦,57◦). A ridge of ILC structures bridges
the gap between the two peaks. In (a) the integrated HI brightness over the velocity range
indicated shows two high-velocity features with center velocities determined to be -127 &
-118 km/s (for the north and south components) straddling the ILC ridge, see text. Frame
(d) shows several HI emission profiles at the latitudes indicated. The HI l,b map of the
striking, unresolved, component at -8 km/s at b = 57◦ is shown in (b). In (c) the area map
of the HI component at -17 km/s is compared to the ILC structure.
– 22 –
Fig. 4.— The elongated ILC structure, peak 33, Table 1, at (l,b) = (89◦, 34.◦5) (contour
levels from 0.03 mK in steps of 0.02 mK) showing a direct relationship to the high-velocity
HI structure in 1 km/s bands at the velocities indicated. The HI structure follows the ILC
structure closely as the center velocity shifts. At -135 and -205 km/s no significant HI
emission is detectable.
– 23 –
Fig. 5.— Further associations between the ILC continuum source 33, Table 1, and HI. (a)
HI profiles toward the ILC peak at the latitude and longitudes indicated. The profile at
longitude 89.◦5 shows excess emission at -40 km/s. The gray-scale representation of this
feature is shown in (b) with the ILC contours overlain. Frame (c) shows the HI data from
(b) in contour form to highlight the similarity to the ILC contours in (b). In (d) the ILC
peak is overlain on the HI emission at low velocities showing the coincidence with a lack of
low velocity emission.
– 24 –
Fig. 6.— ILC peaks 19, 43 & 57 around (l,b) = (165◦, 65.◦5) indicated as contours (from
0.06 to 0.20 mK in intervals of 0.02 mK) in (a) (b) & (d) overlain on inverted gray-scale
images of the HI emission toward high-velocity cloud MI at the velocities indicated. (c)
The location of a soft X-ray excess emission (pixels) with respect to high-velocity cloud MI
contours adapted from Herbstmeier et al. (1995), see text.
	Introduction
	Data and Analysis
	Statistics of the Apparent Associations
	The Angular Distribution of Apparent Associations
	Case Studies of Associated HI and Continuum Structures
	Source 25 at (l,b) = (112.3,57.8): Directly overlapping HI and continuum features
	Sources 11 & 31 centered at (l,b) = (119.5, 57) and association between high- and low-velocity HI
	Continuum source 33 at (l,b) = (89.3, 34.5) and associated high-velocity HI
	Close-up view of HVC MI
	Discussion
	Conclusions
