Wolter-I-like X ray telescope structure using one conical
mirror and one quadric mirror
Shenghao Chen (陈晟昊)
1,2
, Shuang Ma (马 爽)
1,2
, and Zhanshan Wang (王占山)
1,2,
*
1
Key Laboratory of Advanced Micro-Structure Materials, Ministry of Education, Shanghai 200092, China
2
Institute of Precision Optical Engineering, School of Physics Science and Engineering, Tongji University,
Shanghai 200092, China
*Corresponding author: wangzs@tongji.edu.cn
Received September 12, 2016; accepted October 28, 2016; posted online December 1, 2016
Nested multilayer mirrors are commonly used in X ray telescope structure to increase the collecting area. To
balance the difficulty and cost of producing these mirrors, Wolter-I structures are replaced with conical Wolter-I
structures, but these can lead to significantly poorer angular resolutions. In this Letter, we consider changing one
of the mirror shapes (paraboloid or hyperboloid) of a Wolter-I structure to a conical mirror shape, while the other
mirror shape remains a quadric surface-type structure, which can thus ensure the imaging quality. The
cone-hyperboloid structure is nested to obtain on-axis angular resolution and off-axis images.
OCIS codes: 340.7740, 220.2740, 350.1260.
doi: 10.3788/COL201614.123401.
The telescope is an important observation device that
has already produced numerous research results that have
raised scientific awareness of the unknown universe
[1–3]
.
Grazing incidence X ray telescopes are used to study
X ray astronomy, which is a branch of astronomy related
to the observation of X rays from astronomical objects.
Grazing incidence X ray telescope structures were
pioneered by Wolter
[4]
in 1952, when he introduced a
paraboloid-hyperboloid type 1 (Wolter-I) structure that
consisted of a paraboloidal primary mirror and a confocal
hyperboloidal secondary mirror. To increase the collecting
area, Van Speybroeck and Chase
[5]
proposed the concept of
a multilayer nested telescope in 1972. The nested Wolter-I
X ray telescope is an important observation device with a
very high angular resolution that is mounted on satellites,
such as the Chandra X ray observatory
[6–8]
and the XMM-
Newton
[9–11]
. This type of telescope can also focus on
geometrical collection areas, but the fabrication of mirrors
with required quadric surface is highly difficult.
On the basis of the Wolter-I structure, several different
mirror shapes have been optimally designed for different
purposes in the past. To ensure strict satisfaction of the
Abbe sine condition, Wolter
[12]
proposed the Wolter–
Schwarzschild structure in his second Letter, which ex-
actly fulfilled the Abbe sine condition and thus eliminated
the coma aberration for paraxial rays. Werner
[13]
designed
several polynomials with a factor between 2 and 4 for X
ray telescope structures that could improve the angular
resolution. Conconi and Campana
[14]
and Burrows et al.
[15]
determined merit functions that were used to optimize the
polynomials for large-field X ray imaging. Harvey et al.
[16]
designed a telescope with a hyperboloid–hyperboloid
(HH) structure to optimize the angular resolution in the
case of a large field of view. Petre
[17]
and Serlemitsos
[18]
designed cone–cone type-I telescope structures, called
conical Wolter-I telescopes; these are widely used in actual
applications, such as in Suzaku
[19–21]
, NuSTAR
[22–24]
, and
Astro-H
[25–27]
. Saha and Zhang
[28]
simply added a second-
order axial sag to optimize the on-axis image spot of
the conical Wolter-I telescope. The conical Wolter-I tele-
scope has a simple principle: it uses two conical mirrors to
replace the paraboloidal and hyperboloidal surfaces. The
most importa nt advantage of this is that the difficulty and
the cost of fabricating the mirrors both decrease dramati-
cally, and thus, the geometrical collection area can be
increased by the addition of more nested layers. However,
the most serious problem with this structure is that the
angular resolution is significantly worse. Most of these
designs have not been adopted in practical applications,
except the simple conical Wolter-I telescope, because
the complicated mirror shapes make them difficult to fab-
ricate and test. An X ray telescope structure should be
designed with equal importance being given to increasing
the geometrical collection area while ensuring the best
possible angular resolution. At the same time, the diffi-
culty, time, and cost of fabrication of the mirrors must also
be considered.
In this Letter, we consider changing one of the mirror
shapes of the Wolter-I structure to a conical mirror, which
could reduce the production cost in comparison to that
required for a paraboloid mirror or hyperboloid mirror.
The other mirror shape would still have a quadric-type
surface, which includes paraboloid, hyperboloid, and
ellipse shapes, to ensure the imaging quality.
The designs of the cone-hyperboloid (CH), cone-
paraboloid (CP), and cone-ellipse (CE) mirrors are dis-
cussed in this section. The positions of the mirrors can
be calculated based on the Wolter-I telescope structure
that is shown in a schematic diagram in Fig.
1
[29]
. F
1
is
the focus of the paraboloid and the hyperboloid, and F
2
is the other focus of the hyperboloid. f is the focal length
of the telescope. L is the axial length of each mirror.
COL 14(12), 123401(2016) CHINESE OPTICS LETTERS December 10, 2016
1671-7694/2016/123401(5) 123401-1 © 2016 Chinese Optics Letters
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